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Meet the NEW Most Powerful Thing in the Universe · Boring Science

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  Speaker 1: A single object in the universe produces more energy in
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  one second then our Sun will generate across its entire
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  ten billion year lifetime. That's not science fiction. That's happening
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  right now, somewhere in the cosmos, and it's just one
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  contender for the most powerful thing that exists. The universe
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  doesn't do subtle When stars collapse, when galaxies collide, when
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  space itself tears apart at the seams, the energy released
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  makes our most powerful nuclear weapons look like birthday candles.
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  We're talking about forces so extreme they bend reality, twist
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  atoms into impossible shapes, and blast radiation across billions of
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  light years. Here's what makes this question fascinating. Power comes
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  in different forms. A magnetar has a magnetic field so
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  intense it would kill you from a thousand kilometers away
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  by ripping apart the atoms in your body. A quasar
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  shines with the light of a trillion stars from a
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  region smaller than our Solar system. A gamma ray burst
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  releases more energy in seconds than entire galaxies produce in years.
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  So which one wins. The answer depends on how you
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  measure raw energy output sustained power over time. Destructive potential,
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  the ability to warp space itself. Each metric crowns a
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  different champion, and understanding these cosmic titans reveals something profound
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  about how the universe actually works. If you find comfort
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  in these gentle explorations of space and science, I'd be
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  grateful if you'd consider subscribing and giving this video alike.
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  Let's start with the most obvious candidate, quasars. These objects
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  confounded astronomers when they were first discovered sixty years ago.
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  They looked like stars through telescopes, but the math didn't
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  add up. They were impossibly bright and impossibly distant. What
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  astronomers eventually realized changed everything. Quasers aren't stars at all.
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  They're the beating hearts of young galaxies, powered by super
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  massive black holes, consuming matter at a rate that defies comprehension.
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  The fastest growing black hole we found, designated Jay zero
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  five two nine Dash four three five one, has a
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  mass of seventeen billion suns. Every single day, it devours
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  material equivalent to our entire sun. Think about that for
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  a moment. An entire star's worth of matter gone in
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  twenty four hours. And this isn't a quiet process, as
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  that matter spirals toward the black hole, it forms an
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  accretion disc where friction heats the material to millions of degrees.
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  The energy released is staggering. Jay zero five two nine
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  dash four three five one is over five hundred trillion
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  times more luminous than our sun. That number is almost
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  meaningless because our brains can't process it. But here's a
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  comparison that might help. This single object outshines the combined
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  light of every star in the Milky Way by a
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  factor of thousands. Its light has been traveling toward us
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  for over twelve billion years, and it's still bright enough
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  that we can study it in detail. Quasers immit their
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  energy across the entire electromagnetic spectrum, X rays, ultraviolet, visible light,
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  infrared radio waves, all of it pouring out from a
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  region about the size of our solar system. Some quasers
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  generate ten to one hundred times more energy than our
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  entire galaxy, which contains somewhere between two hundred and four
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  hundred billion stars. The physics behind this power is actually elegant.
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  Black Holes are the most efficient engines in the universe
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  for converting mass into energy. Nuclear fusion, the process that
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  powers stars, converts about zero point seven percent of mass
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  into energy. That's what makes the sun shine, But matter
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  falling into a black hole's accretion disk can convert between
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  five point seven percent and thirty two percent of its
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  mass into pure energy before crossing the event horizon. That
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  efficiency is terrifying. It means black holes extract more usable
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  energy from matter than any other process in nature, and
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  when you feed a black hole the mass of a
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  sun every single day, the energy output becomes almost incomprehensible.
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  Scientists recently solved one of the biggest mysteries about quasers,
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  what ignites them. Detailed observations comparing forty eight quasers with
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  over one hundred normal galaxies revealed the trigger quasers are
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  born when galaxies collide. When two galaxies crash together, their
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  gravitational dance pushes enormous amounts of gas toward the supermassive
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  black holes at their centers. This isn't a gentle process.
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  We're talking about hundreds of billions of stars and dust
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  clouds of gas interacting over millions of years. The chaos
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  funnels material inward, feeding the central black hole until it
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  erupts into a quaser. Galaxies hosting quasers are three times
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  more likely to show signs of recent collisions or interactions.
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  The evidence is clear in their distorted shapes, their tidal
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  tales of stars, their warped structures. Violence breeds power. More
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  than nine hundred thousand quasars have been cataloged as of
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  twenty twenty three. They range from six hundred million to
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  thirty billion light years away. The most distant ones show
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  us the universe when it was young, when galaxies were
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  still forming, when collisions were common. Looking at quazas is
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  literally looking back in time to a more more chaotic
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  era of cosmic history. But here's where the competition gets interesting.
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  Quasars are sustained powerhouses, shining continuously for millions of years.
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  Other objects burst onto the scene with even more extreme,
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  if brief, displays of power. Gamma ray bursts are the
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  most violent explosions the universe has produced since the Big
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  Bang itself. They erupt without warning, flooding detectors with the
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  highest energy light known to physics. A typical gamma ray
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  burst releases in mere seconds as much energy as our
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  Sun will generate across its entire ten billion year lifespan.
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  These aren't just bright, they're visible across almost the entire
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  observable universe. When GRB zero eight zero three one nine
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  B detonated seven and a half billion light years away,
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  its optical counterpart reached magnitude five point eight. That's barely
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  visible to the naked eye if you know exactly where
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  to look, Except this star was halfway across the universe.
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  The energy involved is staggering if you assume the explosion
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  radiates equally in all directions. GRB zero eight zero three
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  one nine B released energy within a factor of two
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  of the Sun's entire rest mass energy. That's the energy
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  you'd get if you could somehow convert our Sun entirely
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  into radiation with perfect efficiency, holding nothing back. Gamma ray
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  bursts come in two flavors. Short bursts last less than
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  two seconds and typically result from neutron stars colliding. Long
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  bursts last from two seconds to over a minute and
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  signal the birth of a black hole. When a massive
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  star collapses. On October nine, twenty twenty two, detectors around
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  the world and in orbit all lit up simultaneously. Something
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  had just hammered our solar system with gamma radiation intense
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  enough to overwhelm instruments designed to measure the most powerful
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  events in space. The source, designated GRB two two one
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  zero zero nine A, turned out to be the brightest
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  gamma ray burst ever recorded. The gamma ray emission lasted
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  over three hundred seconds. What makes gamma ray bursts particularly
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  interesting is that astronomers have been missing roughly half their
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  total energy. Recent analysis suggests the energy in a burst's
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  most intense gamma rays equals all its lower energy emissions combined.
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  We've been under counting their power this whole time. The
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  mechanism behind long gamma ray bursts involves hyper nova stellar explosions,
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  an order of magnitude more powerful than regular supernova. When
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  a star more than thirty times the Sun's mass reaches
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  the end of its life, it doesn't go quietly. The
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  core collapses into a black hole, but the outer layers
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  don't just fall in. Conservation of angular momentum causes the
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  collapsing material to form a rapidly rotating disk around the
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  newborn black hole. Jets of material blust outward from the
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  poles at speeds, approaching light itself, punching through the dying
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  star and erupting into space. The first hyper nova ever
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  observed s N nineteen ninety eight BW was one hundred
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  times more luminous than a standard supernova. It was also
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  the first supernova definitively associated with a gamma ray burst,
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  confirming the connection between these extreme stellar deaths and the
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  universe's most powerful explosions. Some hypernova reach truly ridiculous extremes,
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  ASASSN Dash one five l H achieved a peak luminosity
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  approximately five hundred seventy billion times that of our Sun.
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  For comparison, that's twenty times brighter than all the light
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  released by every star in the Milky Way combined, one
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  exploding star outshining an entire galaxy of hundreds of billions
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  of stars. But hypernova and gamma ray bursts, while incredibly powerful,
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  are brief. They flash brilliantly and fade. What about sustained
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  power that isn't quite as intense as quasers but operates
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  on truly cosmic scales. Active galactic nuclei represent and the
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  broader category that includes quasers. AGNs are compact regions at
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  galactic centers that emit tremendous energy not produced by stars.
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  They're the most luminous, persistent sources of electromagnetic radiation in
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  the universe, ranging from relatively modest nearby examples emitting about
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  ten to the forteethh power ergs per second, to distant
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  quasers pumping out more than ten to the forty seventh
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  power ergs per second. That's a range of ten million times.
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  The weakest agn still produces one hundred million times the
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  Sun's power. The strongest outshines our Sun by a factor
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  of ten trillion trillion. A GNS can outshine all the
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  stars in their host galaxy by a factor of one hundred.
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  Imagine that a galaxy containing hundreds of billions of stars
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  and the tiny region at its core produces more light
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  than all of them combined. Most galaxies probably harbour supermassive
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  black holes at their centers. Some of those black holes
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  actively feed, pulling in gas and dust. When they do,
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  they become active galactic nuclei. The feeding process generates jets
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  that can extend for over a million parsecs that's more
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  than three million light years, dwarfing the galaxies themselves. Blazers
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  represent a special subset of AGNs where one of those
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  jets points almost directly at Earth. This creates an illusion
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  called superluminal motion, where features in the jet appear to
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  move faster than light. Measurements of Blazer jets have shown
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  apparent speeds exceeding twenty five times light speed. This isn't
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  real faster than light travel. It's a geometric trick caused
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  by material moving at ninety eight percent of light speed,
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  almost directly toward us, but it demonstrates the extreme velocities involved.
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  These jets accelerate electrons, protons, and atomic nuclei to energies
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  we can barely replicate in our most powerful particle accelerators.
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  Blazers emit extremely high energy gamma rays, light over one
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  hundred million times more energetic than the highest energy X rays.
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  The acceleration mechanisms in these jets remain partially mysterious, but
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  numerical simulations support the possibility of accelerating protons to truly
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  extreme energies. The jets themselves emit across all wavelengths simultaneously,
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  radio waves, microwaves, infrared, visible light, ultraviolet, X rays, gamma rays,
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  all pouring out from a structure that can stretch across
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  millions of light years, all ultimately powered by a supermassive
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  black hole, converting matter into energy with ruthless efficiency. Yet
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  for all this power, for all these cosmic engines producing
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  energies that make stars look dim, there's another class of
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  object that operates on a completely different principle. These objects
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  don't generate their power through accretion or nuclear fusion or
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  matter antimatter annihilation. They generate it through magnetism push to
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  its absolute physical limit. Magnetars are neutron stars, the collapsed
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  cores of dead massive stars, but with magnetic fields so
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  intense they break the rules of normal matter. A typical
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  neutron star has a magnetic field about a triller billion
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  times stronger than Earth's. A magneta's field is a thousand
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  times stronger than that. We're talking about magnetic fields in
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  excess of ten to the fourteenth to ten to the
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  fifteenth gause. For perspective, that's a quadrillion times stronger than
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  Earth's magnetic field. It's the strongest magnetic force ever observed
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  in nature, and it's the most powerful magnetic object detected
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  anywhere in the universe. The field is so intense it
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  dictates the behavior of everything around it. It can twist
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  and distort atoms, stretching them into elongated shapes that shouldn't exist.
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  Hydrogen atoms in a magnetar's field are squashed about two
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  hundred times narrower than normal. The magnetic force overcomes electromagnetic repulsion,
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  the fundamental force that normally can keeps atoms their standard size.
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  This extreme magnetism does something even stranger. It alters the
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  vacuum of space itself. Empty space near a magnetar becomes
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  bi afringent, meaning light waves with different polarizations travel at
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  different speeds. This is a property normally found in certain
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  crystals on Earth, not in the vacuum of space. The
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  magnetic field is so strong it changes the fundamental properties
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  of nothingness. Over time, the crust of a magneta becomes
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  strained by the shifting magnetic field. Underneath the field lines
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  twist and writhe beneath the surface. Eventually, these stresses become
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  too great the crust cracks. What happens next is difficult
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  to comprehend. These starquakes release titanic amounts of energy, sometimes
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  ten to the power of forty six ergs or more
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  in a single outburst. That's more energy released in a
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  fraction of a second than the Sun produces in one
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  hundred thousand years. The explosion can outshine the entire galaxy.
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  On December twenty seventh, two thousand, four, astronomers witnessed one
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  such spectacular blast from the magnetar SGR one eight six
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  dash two O. The burst of gamma rays was so
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  intense it partially ionized Earth's upper atmosphere. From halfway across
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  the galaxy, the energy wave saturated NASA's Swift telescope detectors,
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  instruments specifically designed to observe gamma ray bursts. The spacecraft
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  was essentially blinded by the intensity. At a distance of
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  halfway from Earth to the Moon roughly one hundred ninety
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  two thousand kilometers, the magneta could wipe information from the
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  magnetic stripes of every credit card on Earth. At one
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  thousand kilometers, the magnetic field would be lethal, not through radiation,
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  but through distortion. The field would warp the electron clouds
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  of atoms in your body, rendering the chemistry of life impossible.
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  Your molecules would simply stop functioning as molecules. These objects
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  are only about twenty kilometers in diameter twelve miles across.
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  You could drive around one in less than an hour
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  if you had a road. Yet they pack more mass
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  than our Sun into that impossibly small volume. A tablespoon
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  of magnetar material would weigh over one hundred million tons.
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  But magnetars represent steady state power, constant grinding magnetic energy
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  that persists for than thousands of years. There's another category
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  of cosmic violence that operates on a completely different time scale.
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  These events don't last for millennia. They last for seconds,
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  maybe minutes at most, and in those brief moments they
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  outshine everything. Gamma ray bursts are the most powerful explosions
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  in the universe, not the most energetic over time, the
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  most powerful per unit of time. These are short lived
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  outbursts of the highest energy light, and they can erupt
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  with a quintillion times the luminosity of our Sun. That's
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  a one, followed by eighteen zeros. Almost every day, somewhere
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  in the cosmos, a gamma ray burst occurs without warning.
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  We detect them washing over Earth from distant galaxies. Each
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  one signals something catastrophic, the cataclysm birth of a black
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  hole through either the collapse of a massive star or
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  the merger of neutron stars. A typical gamma ray burst
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  releases as much energy in a few seconds as the
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  Sun will produce in its entire ten billion year lifetime.
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  Think about that ratio ten billion years of solar output
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  compressed into seconds. The explosion can be seen across almost
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  the entirety of the visible universe. Astronomers classify gamma ray
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  bursts into two main types. Short bursts last less than
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  two seconds. Long bursts last two seconds or more, typically
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  about a minute. The mechanism differs between them. Short bursts
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  come from neutron star mergers. Long bursts from the collapse
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  of massive stars into black holes. But here's something researchers
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  discovered recently. We've been missing about half the total energy
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  the gamma rays we detect. The highest energy photons represent
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  only part of the output. The energy in the most
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  intense gamma rays is comparable to all the lower energy
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  emissions combined. Previous measurements were systematically underestimating the true power
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  of these events. GRB zero eight zero three one nine
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  B provides a stark example. This burst occurred seven point
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  five billion light years away. Its optical counterpart, the visible
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  light component, peaked at magnitude five point eight. That's comparable
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  to the dimmest stars you can see with your naked eye.
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  Except this wasn't a star. It was an explosion happening
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  when the universe was roughly half its current age. If
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  you'd been looking at the right spot in the sky
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  at the right moment, you could have seen it without
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  a telescope, a naked eye object from seven point five
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  billion light years away. The energy output was staggering. Assuming
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  a spherical explosion, GRB zero eight zero three one nine
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  B released energy within a factor of two of the
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  rest mass energy of the Sun. That's the energy you'd
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  get if you converted the entire mass of our Sun
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  directly into radiation e equals mc squared taken to its
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  logical extreme. Then came October ninth, twenty twenty two. An
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  intense pulse of gamma radiation swept through our solar system.
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  It overwhelmed detectors on numerous orbiting satellites. The source, designated
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  GRB two two one zero zero nine A for its
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  discovery date, turned out to be the brightest gamma ray
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  burst ever recorded. The gamma ray emission lasted over three
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  hundred seconds five minutes of reality bending power. These events
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  are both extremely energetic and extremely rare, a few per
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  galaxy per million years. The sources are billions of light
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  years away, which tells us something profound about their intrinsic brightness.
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  We're detecting them across cosmic distances that would render entire
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  galaxies invisible. Yet these explosions shine through. Most energy is
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  released in gamma rays, but some bursts have extremely luminous
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  optical counterparts. The visible light alone can outshine billions of stars.
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  The shock waves carry unimaginable kinetic energy, plowing through surrounding
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  space at significant fractions of light speed, but gamma ray
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  bursts are transient seconds to minutes of fury, then silence.
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  There's another class of event that operates on longer time
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  scales while releasing even more total energy. These aren't explosions
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  in the traditional sense. Their eruptions sustained outbursts powered by
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  supermassive black holes feeding at unprecedented rates. In February twenty twenty,
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  astronomers announced the discovery of the Ophiucus supercluster eruption, the
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  most energetic event in the universe ever detected since the
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  Big Bang. It occurred in the Ophiucus cluster in a
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  galaxy designated neve I. The central supermassive black hole consumed
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  nearly two hundred seventy million solar masses of material. That's
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  two hundred seventy million suns worth of gas dust falling
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  into a black hole with a mass of seven billion suns.
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  The eruption lasted about one hundred million years, not seconds,
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  not minutes, one hundred million years of sustained energy output.
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  It released five point seven million times more energy than
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  the most powerful gamma ray burst known. The shock waves
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  and jets of high energy particles punched a cavity in
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  the intra cluster medium the hot gas between galaxies in
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  the cluster. The cavity measures one point five million light
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  years wide, ten times the diameter of the Milky Way.
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  Imagine that scale. A hole in space carved by a
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  single object's feeding frenzy avoid larger than ten of our
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  galaxies placed side by side. MS zero seven three five
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  represents an another example of extreme black hole feeding. Astronomers
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  estimate the central black hole consumed mass equivalent to three
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  hundred million suns. That's as much mass as another supermassive
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  black hole. The energy output was sufficient to create visible
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  structures in the surrounding galaxy cluster. Jets and cavities that
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  will persist for billions of years, long after the feeding
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  event has ended. These aren't just powerful events, their universe
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  altering events. They shape the evolution of galaxy clusters. They
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  regulate star formation across millions of light years. They inject
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  energy and heavy elements into the space between galaxies. Without
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  these violent outbursts, the large scale structure of the cosmos
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  would look completely different. But there's something an even more
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  extreme happening in the universe right now, something that combines
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  the sustained power of these eruptions with intensity that approaches
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  gamma ray burst levels. The fastest growing black hole known
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  to date Jay zero five two nine Dash four three
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  five one, a quasar so luminous it defies comprehension. The
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  central black hole has a mass of seventeen billion suns
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  and its feeding consuming just over one solar mass per day.
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  Every single day, this object swallows mass equivalent to our
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  entire sun. The matter being pulled toward the black hole
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  forms an accretion disc. As material spirals inward, it heats
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  up through friction and compression. The disk emits so much
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  energy that Jay zero five two nine Dash four three
• 28:54
  five one is over five hundred trillion times more luminous
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  than the Sun. The light took over twelve billion years
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  to reach us. We're seeing this object as it was
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  when the universe was less than two billion years old.
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  This is the brightest persistent object in the known universe.
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  Not a brief explosion, not a short lived outburst, constant
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  sustained luminosity at levels that make galaxies look dim. More
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  than nine hundred thousand quasers have been discovered as of
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  twenty twenty three. They range in distance from six hundred
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  million to thirty billion light years away. Quasers emit radiation
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  across the entire electromagnetic spectrum, from X rays to the
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  far infrared, with a peak in the ultraviolet optical bands.
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  Some are strong radio sources. Some emit gamma rays. They
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  can have luminosity between ten and one hundred thousand times
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  that of the Milky Way, generated from a region just
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  a few light days to a few light years across.
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  That's an area comparable in size to our Solar system,
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  producing more light than hundreds of billions of stars. Scientists
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  recently unlocked one of the biggest mysteries about quasers, What
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  triggers them, What causes a super massive black hole to
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  suddenly start feeding at these extreme rates. The answer galaxy collisions.
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  Researchers compared observations of forty eight quasars and their host
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  galaxies with images of over one hundred non quasar galaxies.
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  The conclusion was clear. Galaxies hosting quasars are approximately three
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  times as likely to be interacting or colliding with other galaxies.
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  When two galaxies crashed together, gravitational forces push enormous amounts
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  of gas toward the supermassive black holes at the center
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  of the remnant system. Just before that gas is consumed,
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  it releases extraordinary amounts of energy as radiation. The result
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  is a quasar. The power originates from the efficiency of
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  the conversion process. Accretion disks around super massive black holes
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  can convert between five point seven percent and thirty two
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  percent of an object's mass into energy. Compare that to
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  the zero point seven per cent efficiency of the nuclear
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  fusion process that powers sun like stars. Black Hole accretion
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  is up to forty five times more efficient than stellar
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  fusion at converting mass to energy. This is why quasars
• 31:55
  can have the luminosity of a trillion stars contained in
• 31:59
  a space about the size of our solar system. The
• 32:03
  Milky Way hosts at least one hundred billion stars spread
• 32:06
  across one hundred thousand light years. A quasar concentrates ten
• 32:11
  times that luminosity into a region you could cross in
• 32:15
  a few years at light speed. Observations revealed that quasers
• 32:19
  radiate over a trillion times as much energy as our
• 32:23
  Sun from a region about the size of the Solar System.
• 32:27
  The only mechanism capable of producing such enormous power is
• 32:31
  the conversion of gravitational energy into light by a massive
• 32:36
  black hole. Nothing else works. Nuclear fusion can't do it.
• 32:41
  Matter antimatter annihilation could theoretically match it, but there's no
• 32:46
  plausible source of antimatter in sufficient quantities. The black hole
• 32:51
  explanation isn't just the best answer, it's the only answer
• 32:56
  that fits the observations, which tells us something remarkable about
• 33:00
  the universe. The most powerful persistent objects in existence derive
• 33:07
  their power from gravity, not from nuclear reactions, not from
• 33:12
  electromagnetic forces, from the warping of space time itself around
• 33:18
  the most extreme objects nature allows. But there's another category
• 33:22
  of power in the universe that operates on a completely
• 33:26
  different principle. Quasars shine through sustained accretion. But what about
• 33:32
  objects whose power comes not from how much energy they emit,
• 33:37
  but from how intensely they can warp reality itself. Enter magnetars.
• 33:43
  These are neutron stars, the collapsed cores of massive stars
• 33:48
  that went super and ova. About twenty kilometers in diameter,
• 33:53
  roughly one point four solar masses compressed into a sphere
• 33:57
  the size of a city. A tablespoon of magnetore material
• 34:03
  would have a mass of over one hundred million tons.
• 34:08
  That density alone is extreme. But it's not the density
• 34:12
  that makes magnetars remarkable. It's the magnetic field. A magnetar's
• 34:19
  magnetic field reaches intensities between ten to the fourteenth and
• 34:24
  ten to the fifteenth gausse. That's a quadrillion times stronger
• 34:29
  than Earth's magnetic field, one hundred million times stronger than
• 34:34
  any magnet humans have ever created. As of twenty twenty,
• 34:40
  magnetars are the most powerful magnetic objects detected anywhere in
• 34:45
  the universe. How strong is that field? In practical terms,
• 34:50
  At a distance halfway between Earth and the Moon roughly
• 34:54
  one hundred ninety two thousand kilometers away, a magnetar could
• 34:59
  wipe the magnet magnetic information from every credit card. On Earth,
• 35:04
  every hard drive, every magnetic storage device erased from nearly
• 35:12
  two hundred thousand kilometers away. At one thousand kilometers distance,
• 35:18
  the magnetic field would be lethal, not from radiation from
• 35:23
  the field itself. The magnetic forces would distort the electron
• 35:28
  clouds in your atoms. Hydrogen atoms would be squashed two
• 35:32
  hundred times narrower than normal. The chemistry that makes life
• 35:37
  possible would simply stop working. Your molecular bonds would fail.
• 35:43
  You would cease to exist as a coherent biological entity.
• 35:47
  The field alters the vacuum of space itself. Empty space
• 35:52
  near a magnetar becomes biafringent, splitting light into two polarization
• 35:58
  states like certain crystals do on Earth. The quantum vacuum,
• 36:04
  normally isotropic and uniform, becomes directional and structured. The magnetic
• 36:10
  field is so intense it dictates how virtual particles pop
• 36:14
  in and out of existence. This isn't just strong magnetism.
• 36:19
  This is magnetism powerful enough to rewrite the rules of
• 36:23
  quantum field theory. In its vicinity, magnetars form when stars
• 36:29
  between ten and twenty five solar masses collapse. The compression
• 36:35
  during the collapse can supercharge any pre existing magnetic field
• 36:39
  in the stellar core. The result is a field that's
• 36:43
  roughly one thousand times stronger than a normal neutron star,
• 36:48
  and neutron stars already have magnetic fields billions of times
• 36:52
  stronger than anything on Earth. But the most spectacular displays
• 36:57
  of magnetar power come from Stark. Over time, the magnetar's
• 37:03
  crust becomes strained. The magnetic field beneath the surface shifts
• 37:07
  and evolves. The crust, solid but under tremendous stress, eventually
• 37:14
  can't handle the strain. It cracks, and when it does,
• 37:18
  the energy release is staggering. A single starquake can release
• 37:22
  ten to the forty six ergs of energy that's more
• 37:26
  energy than the Sun produces in one hundred thousand years,
• 37:30
  released in a fraction of a second. December twenty seventh,
• 37:34
  two thousand four, the magnetar SGR one eight six DASH
• 37:40
  two oh, located about fifty thousand light years away halfway
• 37:45
  across the galaxy, experienced a massive star quake. The burst
• 37:51
  of gamma rays that reached Earth was so intense it
• 37:54
  partially ionized our upper atmosphere. From halfway across the Milky Way,
• 38:01
  the radiation overwhelmed detectors on multiple satellites, including NASA's Swift telescope,
• 38:08
  specifically designed to observe gamma ray bursts. For a tenth
• 38:13
  of a second, this object became the brightest source of
• 38:17
  gamma rays in the sky, outshining every other object in
• 38:22
  the universe in that energy range, despite being fifty thousand
• 38:27
  light years away. If SGR one eight zero six dash
• 38:32
  two zero had been located just ten light years from Earth,
• 38:37
  the distance to some of our nearest stellar neighbours, that
• 38:41
  burst would have caused a mass extinction event. The radiation
• 38:46
  would have stripped away a significant portion of Earth's ozone layer.
• 38:52
  The aftermath would have been catastrophic for life on the surface.
• 38:57
  Magnetars demonstrate that power in the U S universe doesn't
• 39:01
  always come from size or luminosity. Sometimes it comes from intensity,
• 39:08
  from the concentration of fundamental forces into configurations so extreme
• 39:13
  they border on impossible. But even magnetars, for all their
• 39:18
  magnetic intensity, operate continuously. Their power output is constant, sustained
• 39:25
  over millions of years as they slowly spin down and
• 39:29
  their magnetic fields decay. What about events that release comparable
• 39:33
  energy in seconds? Gamma ray bursts. These are the most
• 39:38
  powerful explosions in the universe, since the Big Bang itself.
• 39:43
  Short lived outbursts of the highest energy photon's nature produces.
• 39:48
  They can erupt with the quintillion times the luminosity of
• 39:52
  our Sun. That's a one, followed by eighteen zeros. A
• 39:57
  typical gamma ray burst releases as much energy in a
• 40:01
  few seconds as the Sun will produce over its entire
• 40:05
  ten billion year lifetime. Almost every day, somewhere in the
• 40:10
  observable universe, a gamma ray burst occurs. We detect them
• 40:15
  as pulses of high energy radiation washing over Earth from
• 40:20
  random directions in the sky. Each one marks the birth
• 40:24
  of a black hole, either from the collapse of a
• 40:28
  massive star or from the merger of two neutron stars.
• 40:33
  Astronomers classify gamma ray bursts into two categories based on duration.
• 40:38
  Short bursts last less than two seconds. Long bursts last
• 40:43
  two seconds or more, typically about a minute. The mechanism differs.
• 40:48
  Short bursts come from neutron star mergers. Long bursts come
• 40:53
  from collapsing massive stars events called hypernovae. Because gamma ray burs,
• 41:00
  USTs originate billions of light years away, the fact we
• 41:04
  can detect them at all, tells you how powerful they are.
• 41:09
  These explosions can be seen across nearly the entire observable universe.
• 41:15
  Light from a gamma ray burst can travel for thirteen
• 41:19
  billion years and still be bright enough to trigger our instruments.
• 41:24
  The energy output is concentrated into two narrow jets material
• 41:30
  streaming out at ninety nine point ninety nine percent the
• 41:33
  speed of light, powered by the newborn black hole at
• 41:37
  the center. If you're in the path of one of
• 41:40
  those jets, you see a gamma ray burst. If you're
• 41:44
  off to the side, you might see a supernova, or
• 41:47
  you might see nothing at all, depending on the angle.
• 41:52
  Recent observations revealed something unexpected. The energy in the most
• 41:57
  intense gamma rays from a burst is comparable to all
• 42:01
  the lower energy emissions combined. Astronomers had been missing roughly
• 42:06
  half the total energy output. The bursts are even more
• 42:10
  powerful than we thought. GRB zero eight zero three one
• 42:15
  nine B, detected in two thousand and eight, was accompanied
• 42:19
  by an optical flash that peaked at magnitude five point
• 42:23
  eight that's visible to the naked eye from seven point
• 42:28
  five billion light years away. If you had been looking
• 42:32
  at exactly the right spot in the sky at exactly
• 42:35
  the right moment. You could have seen this explosion with
• 42:39
  your unaided eyes, despite it occurring when the universe was
• 42:43
  barely half its current age, The energy output of GRB
• 42:48
  zero eight zero three one nine B, assuming spherical emission,
• 42:53
  was within a factor of two of the total rest
• 42:56
  mass energy of the Sun. Essentially, if you converted the
• 43:01
  Sun's entire mass to energy, you'd get approximately the output
• 43:06
  of that single gamma ray burst, except the burst released
• 43:11
  it in seconds, not over ten billion years. October ninth,
• 43:16
  twenty twenty two brought GRB two two one zero zero
• 43:20
  nine A, the brightest gamma ray burst ever recorded. Satellites
• 43:26
  across the Solar System registered the event. The gamma ray
• 43:30
  emission lasted over three hundred seconds. The energy output was
• 43:34
  so extreme it saturated multiple detector systems designed to measure
• 43:39
  these events. Astronomers immediately recognized this as exceptional. GRB two
• 43:46
  two one zero zero nine A occurred relatively nearby by
• 43:51
  cosmic standards, about two point four billion light years away.
• 43:56
  The combination of proximity and intrinsic brightness made it the
• 44:00
  most energetic electromagnetic event ever observed. But gamma ray bursts,
• 44:06
  despite their extreme power, are brief seconds or minutes, then
• 44:12
  they fade. The afterglow can persist for days or weeks,
• 44:18
  but the main event is fleeting. There's something even more powerful,
• 44:24
  not in terms of instantaneous energy output, but in total
• 44:29
  energy released over time, the Opfucus supercluster eruption. February twenty twenty,
• 44:36
  astronomers announced the discovery of what remains the most energetic
• 44:40
  event ever detected in the universe since the Big Bang.
• 44:45
  It occurred in the Ofucus galaxy cluster, in a galaxy
• 44:50
  designated NEIVE one. The cause was a supermassive black hole
• 44:55
  with a mass of about seven billion solar masses. Over
• 45:00
  approximately one hundred million years, this black hole accreted nearly
• 45:05
  two hundred seventy million solar masses of material. The energy
• 45:10
  released during this prolonged feeding frenzy created a cavity in
• 45:15
  the surrounding intracluster medium about one point five million light
• 45:20
  years wide, ten times the diameter of the Milky Way.
• 45:24
  The eruption released five point seven million times more energy
• 45:28
  than the most powerful gamma ray burst known, not in
• 45:32
  seconds over millions of centuries, but the total energy budget
• 45:37
  exceeded anything else we've observed. The eruption sent shock waves
• 45:42
  and jets of particles tearing through the hot gas between
• 45:46
  galaxies and the cluster. It displaced enormous volumes of material.
• 45:52
  The cavity it carved out is visible in X ray
• 45:56
  images as a dark region, a whole punched in the
• 46:00
  glowing gas that fills the space between galaxies. Similar events
• 46:05
  have been observed in other galaxy clusters. MS zero seven
• 46:10
  three five consumed an estimated three hundred million solar masses.
• 46:15
  That's as much mass as another supermassive black hole. The
• 46:19
  energy required to move that much material to carve out
• 46:23
  voids millions of light years across exceeds the total energy
• 46:29
  output of entire galaxies over billions of years. These cluster
• 46:34
  eruptions represents sustained power on scales that dwarf almost everything else.
• 46:40
  They're driven by the same mechanism as quasars accretion onto
• 46:45
  supermassive black holes, but they operate over longer time scales
• 46:50
  and involve even more mass. Yet, there's one more category
• 46:54
  of extreme power that deserves attention. Not the power to
• 46:59
  emit light or to warp space with magnetic fields, but
• 47:03
  the power to literally shake the fabric of space time
• 47:07
  itself merging supermassive black holes. When two black holes with
• 47:13
  masses of one hundred million solar masses each spiral into
• 47:18
  one another and merge, the final moment of coalescence releases
• 47:23
  gravitational waves. These ripples in space time carry away enormous
• 47:28
  amounts of energy in the last second before merger. The
• 47:34
  energy emitted as gravitational waves can be thousands of times
• 47:37
  greater than the combined electromagnetic output of every star in
• 47:42
  the observable universe, thousands of times in one second. This
• 47:49
  isn't light, it's not matter, it's not even radiation in
• 47:53
  the conventional sense. It's the geometry of space time itself oscillating,
• 48:00
  carrying away the rotational energy of the merging black holes.
• 48:05
  The power output during that final second exceeds anything else
• 48:10
  in nature, but you can't see it with a telescope.
• 48:14
  You need gravitational wave detectors instruments like Ligo and virgo
• 48:20
  that measure the infinitesimal stretching and compressing of space as
• 48:25
  these waves pass through Earth. The waves from merging supermassive
• 48:30
  black holes are too low in frequency for current detectors,
• 48:36
  we can observe stellar mass black hole mergers roughly ten
• 48:40
  to one hundred solar masses. Future space based detectors like
• 48:45
  Lisa will be able to detect the supermassive mergers. When
• 48:50
  they do, will be observing the most powerful events in
• 48:53
  the universe, not in electromagnetic radiation in pure gravitational energy.
• 49:01
  Power in the universe comes in many forms, sustained luminosity
• 49:06
  from quasars, intense magnetic fields from magnetars, explosive gamma ray bursts,
• 49:14
  prolonged eruptions from supermassive black holes, gravitational waves from merging
• 49:20
  compact objects. Each represents a different way the universe concentrates energy.
• 49:27
  Each pushes against the limits of what physics allows, and
• 49:31
  each reminds us that the cosmos operates at scales and
• 49:36
  intensities that challenge human comprehension. The universe doesn't just have
• 49:42
  one answer for most powerful. It has categories distinctions that matter.
• 49:49
  Power measured by light output points to quasers, power measured
• 49:54
  by magnetic intensity points to magnetars, power measured by explosive
• 49:59
  energy release points to gamma ray bursts, and power measured
• 50:04
  by gravitational waive emission points to merging black holes. But
• 50:09
  there's another dimension worth examining, sustained versus instantaneous power. Gamma
• 50:16
  ray bursts release staggering amounts of energy, but they're over
• 50:20
  in seconds, maybe a few minutes. For the longest ones,
• 50:25
  the power output during those brief moments exceeds almost anything else,
• 50:32
  but the total energy budget integrated over time might be
• 50:37
  less than what a quasar emits over years or centuries.
• 50:41
  Quasers sustain their luminosity for millions of years, their beacons
• 50:47
  that shine across cosmic time. A quaser that radiates at
• 50:52
  ten to the forty seventh power ergs per second for
• 50:55
  a million years delivers far more total energy than a
• 50:59
  gamma ray burst that lasts thirty seconds, even though the
• 51:04
  burst's peak power is higher. This distinction matters when comparing objects.
• 51:11
  Are we talking about peak power or total energy output.
• 51:16
  Peak power favors transient events merging black holes in their
• 51:21
  final second, gamma ray bursts, hypernovae. Total energy favours sustained
• 51:30
  sources quasers, active galactic nuclei, the prolonged eruptions in galaxy clusters.
• 51:39
  Neither measure is more correct. They're different ways of quantifying power,
• 51:44
  and the universe produces extremes in both categories. Let's focus
• 51:49
  on one object that combines sustained power with extraordinary scale,
• 51:54
  The fastest growing black hole ever discovered. J zero five
• 51:59
  two Dash four three five one. This quaser holds the
• 52:04
  record for luminosity. It's the brightest object in the known universe,
• 52:09
  not the most powerful in terms of peak energy release,
• 52:13
  but the brightest steady source we've observed. The black hole
• 52:18
  at its center has a mass of seventeen billion solar masses.
• 52:23
  That alone places it among the most massive black holes known.
• 52:28
  But mass isn't what makes it remarkable. It's the feeding rate.
• 52:33
  This black hole consumes more than one solar mass per day.
• 52:38
  Every day it swallows material equivalent to our entire sun.
• 52:42
  The accretion disc surrounding it glows so intensely that the
• 52:46
  quasar outshines everything else. Jay zero five two nine Dash
• 52:52
  four three five one is over five hundred trillion times
• 52:57
  more luminous than the sun. Let that number settle half
• 53:03
  a quadrillion times brighter than the star that lights our world.
• 53:08
  From an object roughly the size of our solar system,
• 53:12
  the light from this quaser has traveled for over twelve
• 53:15
  billion years to reach us. We're seeing it as it
• 53:19
  was when the universe was less than two billion years old,
• 53:24
  shortly after the first galaxies formed. Yet even across that
• 53:29
  vast distance, across billions of light years of expanding space,
• 53:34
  it's still the brightest thing we've detected. This raises an
• 53:39
  obvious question, how did such a massive black hole grow
• 53:43
  so quickly in the early universe. We don't have a
• 53:47
  complete answer. Black Holes this large shouldn't exist so soon
• 53:52
  after the Big Bang, at least not according to standard
• 53:56
  growth models. A black hole grows by a creting matter,
• 54:00
  but accretion has limits. When matter falls onto a black hole,
• 54:05
  it heats up, it radiates That radiation creates outward pressure.
• 54:12
  Radiation pressure pushes against infalling material. This creates a natural
• 54:18
  limit called the Eddington limit. A black hole can only
• 54:22
  grow so fast before its own luminosity prevents additional matter
• 54:26
  from falling in. The radiation blows away the surrounding gas.
• 54:32
  For j zero five two nine dash four three five one,
• 54:36
  to reach seventeen billion solar masses in less than two
• 54:40
  billion years requires accretion rates near or above the Eddington
• 54:45
  limit for extended periods. That's theoretically possible, but rare, and
• 54:51
  it doesn't fully explain how the seed black hole formed
• 54:55
  in the first place. Some models propose that the early
• 54:59
  universe conditions favoring rapid black hole growth, dense gas clouds,
• 55:05
  high merger rates, less feedback from stellar winds, but we're
• 55:11
  still working out the details. What we do know is
• 55:14
  that Jay zero five two nine Dash four three five
• 55:18
  one exists and it's feeding voraciously. The accretion disk converts
• 55:25
  mass to energy with extraordinary efficiency. Between five point seven
• 55:31
  percent and thirty two percent of the infalling mass gets
• 55:35
  converted to radiation, depending on the black hole's spin and
• 55:40
  the disk's properties. Nuclear fusion in stars converts about zero
• 55:45
  point seven percent of mass to energy. Accretion onto black
• 55:50
  holes is far more efficient. It's the most efficient energy
• 55:54
  conversion process in nature aside from matter antimatter annihilation. This
• 56:01
  efficiency is why quasas can outshine entire galaxies. The black
• 56:07
  hole at the center of a quasa might be millions
• 56:10
  or billions of solar masses, but the accretion disc is
• 56:15
  relatively small, just light days to light years across, Yet
• 56:21
  it produces more light than hundreds of billions of stars.
• 56:26
  The power comes from gravitational energy. Matter falling into a
• 56:31
  black hole releases its gravitational potential energy. That energy heats
• 56:36
  the accretion disc to millions of degrees hot enough to
• 56:40
  emit X rays and ultraviolet light. The disc doesn't just glow,
• 56:46
  It launches jets, streams of particles accelerated to near light speed.
• 56:53
  These jets extend for millions of light years. In some cases,
• 56:58
  they punch through the surrounding gases, creating enormous bubbles and cavities.
• 57:04
  Quasers were common in the early universe. More than nine
• 57:08
  hundred thousand have been catalogued. Most are billions of light
• 57:12
  years away. We're seeing them as they were when the
• 57:16
  universe was young. Today quasers are rarer. Most supermassive black
• 57:22
  holes have consumed the available gas in their vicinity their
• 57:26
  dormant quiet. The Milky Way's central black hole falls into
• 57:31
  this category. Sagittarius a star is massive but currently inactive.
• 57:39
  It's not feeding at rates that produce quaser level luminosity,
• 57:43
  but quasers can be reawakened. When galaxies collide, gravitational forces
• 57:49
  funnel gas toward the central black holes. This can trigger
• 57:54
  a new phase of accretion, a new quaser observations show
• 57:59
  that gallant Uxi's hosting quasers are about three times more
• 58:04
  likely to be interacting or colliding with other galaxies. The
• 58:09
  connection between galaxy mergers and quasar activity is well established.
• 58:15
  This tells us something important. The most powerful sustained objects
• 58:20
  in the universe are triggered by cosmic violence. Galaxies don't
• 58:25
  produce quasers in isolation. They need disruption interaction. The chaos
• 58:32
  of collision funnels fuel to the black hole. Without that
• 58:36
  fuel supply, even the most massive black holes remain dark.
• 58:41
  J zero five two nine Dash four three five one
• 58:47
  is likely the product of such processes. Its host galaxy
• 58:51
  probably experienced multiple mergers. Each merger delivered fresh gas to
• 58:56
  the central black hole. Each accretion event increase the black
• 59:00
  hole's mass and luminosity, and the cycle continues as long
• 59:06
  as gas keeps falling in the quasar keeps shining. But
• 59:10
  even Jay zero five two nine Dash four three five
• 59:14
  one won't last forever. Eventually, the gas supply will deplete,
• 59:20
  the accretion rate will drop, the luminosity will fade, the
• 59:25
  black hole will enter a quiet phase, like Sagittarius a star.
• 59:31
  This raises another question, what was the most luminous quasar
• 59:36
  that ever existed. We can only observe quasars whose light
• 59:40
  has reached us. There could be even brighter quasars at
• 59:43
  distances so great their light hasn't arrived yet, or quasars
• 59:48
  that existed briefly and faded before we could detect them.
• 59:53
  The universe is thirteen point eight billion years old. We
• 59:58
  can only see objects who light has had time to
• 1:00:01
  cross space and reach our telescopes. This creates an observational horizon.
• 1:00:08
  Beyond that horizon, there are regions of the universe we
• 1:00:12
  can never observe, not because they don't exist, but because
• 1:00:17
  the light hasn't had time to travel the distance. Some
• 1:00:22
  of those regions might host quasars even more luminous than
• 1:00:26
  Jay zero five two nine dash four three five one.
• 1:00:32
  We'll never know. This limitation applies to all astronomy. We're
• 1:00:37
  constrained by the speed of light and the age of
• 1:00:40
  the universe. But within the observable universe, Jay zero five
• 1:00:45
  two nine dash four three five one currently holds the record,
• 1:00:51
  and it's a worthy champion. Its luminosity dwarfs everything else
• 1:00:55
  we've cataloged. It represents the extreme end of sustain A
• 1:01:01
  black hole feeding at maximum capacity, converting mass to light
• 1:01:06
  with ruthless efficiency. Yet even this extraordinary object has competition
• 1:01:12
  in different categories of power. If we shift from electromagnetic
• 1:01:16
  radiation to other forms of energy, different objects take the lead.
• 1:01:22
  Magnetars dominate magnetic field strength, Gamma ray bursts dominate explosive
• 1:01:29
  energy release, merging black holes dominate gravitational wave emission. And
• 1:01:35
  then there are objects that combine multiple extremes. Blazers, for instance,
• 1:01:41
  A blazer is a quasar with its jet pointed directly
• 1:01:45
  at us. The relativistic jet, traveling at nearly light speed,
• 1:01:50
  is aimed straight at Earth. This creates an effect called
• 1:01:54
  relativistic beaming. When a jet moves toward you at close
• 1:01:59
  to light speed, its radiation gets concentrated in the forward direction.
• 1:02:05
  The light gets compressed, blue shifted, amplified. What you see
• 1:02:10
  is far brighter than if the jet were pointed elsewhere.
• 1:02:14
  Blazars can appear extraordinarily luminous, not because they're intrinsically more
• 1:02:20
  powerful than other quasars, but because the geometry favors our
• 1:02:25
  line of sight. But some blazars are genuinely extreme. They
• 1:02:30
  emit gamma rays at energies exceeding one hundred billion electron volts.
• 1:02:36
  That's light more than one hundred million times more energetic
• 1:02:40
  than medical X rays. These high energy photons are created
• 1:02:46
  when particles in the jet collide with lower energy photons.
• 1:02:51
  The collisions boost the photon energies to extreme levels. Blazers
• 1:02:56
  also exhibit superluminal motion. Features in the jet appear to
• 1:03:01
  move faster than light across the sky. This is an
• 1:03:05
  illusion caused by the jets orientation and speed. The material
• 1:03:11
  isn't actually exceeding light speed, but the apparent motion can
• 1:03:15
  be twenty five times faster than light. The true speed
• 1:03:20
  is typically above ninety eight per cent of light speed,
• 1:03:25
  close enough to the cosmic speed limit that relativistic effects dominate.
• 1:03:30
  Blazers challenge our instruments. Their gamma ray emissions are so
• 1:03:35
  intense they can saturate detectors designed to observe the highest
• 1:03:39
  energy events in the universe. They are also variable. Blazer
• 1:03:45
  luminosity can change on time scales of hours or days.
• 1:03:49
  The jets activity fluctuates, the particle acceleration varies, the radiation
• 1:03:56
  outputs surges and drops. This variability tells us something about
• 1:04:01
  the jets structure, the emitting region must be compact. If
• 1:04:06
  the gamma rays came from a region light years across,
• 1:04:09
  we wouldn't see fluctuations on our long timescales. Light travel
• 1:04:15
  time would smooth out the variations, but if the emitting
• 1:04:19
  region is only light hours or light days across, rapid
• 1:04:24
  changes are possible. The jet can vary quickly because the
• 1:04:29
  entire emitting zone can respond coherently. This makes blazers useful
• 1:04:35
  probes of black hole physics. By watching how quickly the
• 1:04:39
  luminosity changes, we can in further size and structure of
• 1:04:43
  the jet. We can study particle acceleration in extreme magnetic fields.
• 1:04:49
  We can test theories of relativistic plasma behavior, and we
• 1:04:54
  can appreciate that the universe contains objects capable of accelerating
• 1:04:59
  part of to energies we can barely reproduce in our
• 1:05:03
  largest colliders. The jets from supermassive black holes are cosmic
• 1:05:09
  particle accelerators operating at scales and powers we can't match.
• 1:05:15
  Some blazars are also neutrino sources. Neutrinos are ghostly particles
• 1:05:21
  that rarely interact with matter. They pass through planets, stars,
• 1:05:26
  even entire galaxies without stopping, but occasionally a neutrino will
• 1:05:32
  collide with an atom in a detector buried deep underground
• 1:05:36
  or under Antarctic ice. When that happens, we can trace
• 1:05:41
  the neutrino back to its source. In twenty seventeen, a
• 1:05:46
  neutrino detected by ice Cube, a detector embedded in Antarctic ice,
• 1:05:51
  was traced to a blazer called tx S zero five
• 1:05:55
  zero six plus zero five six. This was the first
• 1:06:00
  time a high energy neutrino was conclusively linked to a
• 1:06:03
  specific cosmic source. It confirmed that blazars produce not just
• 1:06:08
  gamma rays, but also neutrinos. The particle acceleration in the
• 1:06:14
  jet is so extreme it creates neutrinos with energies far
• 1:06:18
  exceeding anything from the Sun or other normal stars. This
• 1:06:23
  multi messenger astronomy, combining light, gravitational waves, and neutrinos, opens
• 1:06:30
  new ways to study the most powerful objects. Each messenger
• 1:06:34
  carries different information. Light tells us about temperature and composition,
• 1:06:40
  Gravitational waves tell us about spacetime distortion. Neutrinos tell us
• 1:06:46
  about particle interactions in extreme environments. Together, they reveal a
• 1:06:53
  universe far more dynamic and violent than visible light alone suggests,
• 1:06:59
  and they conform firm what the numbers already told us.
• 1:07:03
  The most powerful objects in the universe operate at energy
• 1:07:07
  scales that dwarf human experience. They challenge our instruments, They
• 1:07:13
  push against theoretical limits. They remind us that the cosmos
• 1:07:17
  is not a gentle place. Power in the universe is
• 1:07:21
  not evenly distributed. Most of space is cold, dark, nearly empty.
• 1:07:27
  But in rare locations, under specific conditions, energy concentrates black holes,
• 1:07:33
  form jets, launch magnetic fields, amplify explosions occur. These rare
• 1:07:39
  events and objects dominate the energy budget of the universe.
• 1:07:44
  They shape galactic evolution. They enrich the interstellar medium with
• 1:07:49
  heavy elements. They trigger star formation, They regulate gas flows
• 1:07:54
  across cosmic scales. Without quasas, without gamma ray bursts, without
• 1:08:00
  supernova and magnetars, and all the other extreme phenomena, galaxies
• 1:08:05
  would evolve differently, structure formation would follow different pathways. The
• 1:08:12
  universe would look different. The most powerful objects aren't just
• 1:08:17
  interesting curiosities. They're essential players in cosmic history, and they
• 1:08:22
  define what's possible in the universe. Now you're probably wondering something.
• 1:08:28
  If black holes and their jets dominate the power rankings,
• 1:08:32
  what about other extreme objects? What about the densest stars?
• 1:08:38
  What about magnetic fields so strong they warp the fabric
• 1:08:41
  of reality itself? Enter magnetars. Magnetars are neutron stars, but
• 1:08:48
  calling them that is like calling a supernova a bright light.
• 1:08:53
  Their neutron stars with magnetic fields so powerful they redefine
• 1:08:58
  what we mean by strong. A typical neutron star has
• 1:09:03
  a magnetic field about a trillion times stronger than Earth's,
• 1:09:07
  already absurd, already beyond human scale. A magnetar multiplies that
• 1:09:14
  by another thousand, the numbers become almost meaningless. A magnetar's
• 1:09:20
  magnetic field reaches ten to the fourteenth gass, sometimes ten
• 1:09:25
  to the fifteenth. That's a quadrillion times stronger than Earth's field.
• 1:09:31
  The strongest magnetic field humans have ever created in a
• 1:09:35
  laboratory peaks around a million gaus. A magnetar's field is
• 1:09:40
  one hundred million times stronger than that. What does a
• 1:09:44
  field like that actually do? It distorts atoms Hydrogen, the
• 1:09:49
  simplest element gets compressed to a fraction of its normal width.
• 1:09:54
  The electron orbits stretch and deform under the magnetic stress,
• 1:10:00
  Chemistry as we know it stops working. At a distance
• 1:10:04
  of a thousand kilometers, a magneto's field would be lethal,
• 1:10:09
  not because of radiation, though there's plenty of that, because
• 1:10:14
  the magnetic field itself would tear apart the electron clouds
• 1:10:18
  in your atoms. The biochemistry that keeps you alive would
• 1:10:23
  simply cease to function. Closer in, things get stranger. The
• 1:10:28
  magnetic field becomes so intense it affects the vacuum of space.
• 1:10:33
  Empty space under normal conditions is isotropic. Light travels the
• 1:10:38
  same speed in all directions, but near a magnetar, the
• 1:10:43
  vacuum becomes biofringent. Light polarized in different directions, travels at
• 1:10:49
  different speeds. Space itself develops properties we normally associate with crystals.
• 1:10:56
  This isn't theoretical, We've measured it. The power output of
• 1:11:02
  a magnetar doesn't come from fusion. Neutron stars don't fuse anything,
• 1:11:08
  their cares are too dense. Instead, magnetars get their energy
• 1:11:13
  from their magnetic fields. As the field decays over thousands
• 1:11:17
  of years, it releases energy the star's crust under immense
• 1:11:23
  strain from the shifting field lines occasionally cracks. These are
• 1:11:28
  called starquakes. The name sounds almost gentle. It's not a
• 1:11:34
  typical starquake on a magnetar releases more energy in a
• 1:11:38
  fraction of a second than the Sun produces in ae
• 1:11:42
  hundred thousand years. That's ten to the forty sixth ergs.
• 1:11:47
  To put that in perspective, if you could somehow convert
• 1:11:51
  a single kilogram of matter entirely into energy, you'd get
• 1:11:55
  about ten to the twenty first ergs. A magnet t
• 1:12:00
  tar starquake releases energy equivalent to converting ten billion trillion
• 1:12:05
  kilograms of matter into pure radiation in a tenth of
• 1:12:09
  a second. December twenty seventh, two thousand and four, a
• 1:12:14
  magnetar called SGR one eight zero six DASH two zero
• 1:12:20
  had one of these outbursts. The gamma ray pulse was
• 1:12:23
  so intense its saturated detectors on satellites designed specifically to
• 1:12:29
  measure gamma ray bursts. The pulse traveled fifty thousand light
• 1:12:34
  years across the galaxy. When it hit Earth's upper atmosphere,
• 1:12:39
  it partially ionized the ionosphere from halfway across the Milky Way,
• 1:12:44
  a stellar object the size of a city temporarily disrupted
• 1:12:48
  our planet's atmospheric chemistry. If that magnetar had been ten
• 1:12:53
  light years away instead of fifty thousand, the burst would
• 1:12:57
  have triggered a mass extinction. Magnetars exist because of how
• 1:13:02
  neutron stars form. When a massive star collapses, conservation of
• 1:13:07
  angular momentum spins up the core. Conservation of magnetic flux
• 1:13:13
  amplifies the field. If the original star had even a
• 1:13:18
  modest magnetic field, the collapse concentrates it. The field lines
• 1:13:24
  frozen into the stellar material compress along with everything else.
• 1:13:28
  The result is a star twenty kilometers across with a
• 1:13:31
  mass one point four times the sun. The density is
• 1:13:35
  so extreme that a tea spoon of neutron star material
• 1:13:39
  would weigh one hundred million tons on Earth. The magnetic
• 1:13:42
  field threading through this ultra dense matter reaches levels that
• 1:13:47
  simply don't exist anywhere else in nature. The field energy
• 1:13:51
  alone contributes measurably to the star's gravitational mass. But here's
• 1:13:56
  what makes magnetars particularly interesting for our discacushion about power.
• 1:14:02
  They're not the most luminous objects quasas outshine them by
• 1:14:06
  enormous margins. They're not the most energetic events gamma ray
• 1:14:12
  bursts release more total energy. But magnetars have the strongest
• 1:14:18
  magnetic fields ever measured in the universe, and magnetic fields
• 1:14:23
  are a form of power. They can accelerate particles, they
• 1:14:27
  can store energy, They can do work across vast distances.
• 1:14:32
  A magnetar sitting in empty space doesn't just radiate. It
• 1:14:37
  creates a magnetosphere extending thousands of kilometers outward. Any charged
• 1:14:43
  particle entering that region gets accelerated to relativistic speeds. The
• 1:14:48
  field lines twist and snap, releasing bursts of X rays
• 1:14:52
  and gamma rays. The star essentially becomes a particle accelerator,
• 1:14:58
  operating continuously for Mali Lena. This matters for how we
• 1:15:02
  think about power distribution in the universe. Quasers and blazers
• 1:15:07
  represent one mode, accretion onto supermassive black holes, converting gravitational
• 1:15:15
  potential energy into radiation and kinetic energy of jets. Gamma
• 1:15:21
  ray bursts represent another, explosive events releasing stored energy all
• 1:15:28
  at once. Magnetars represent a third mode, sustained power from
• 1:15:33
  magnetic field decay. It's a different mechanism entirely, no accretion,
• 1:15:38
  disc no jet, just a magnetic field. So strong, It
• 1:15:43
  dominates the local environment and radiates energy as it slowly unwinds.
• 1:15:49
  And here's something you might not expect. Magnetars probably aren't
• 1:15:54
  that rare. We found about thirty confirmed magnetars in the
• 1:15:58
  Milky Way, but our galaxy is big, and magnetars are
• 1:16:03
  hard to detect unless they're actively flaring. The estimated population
• 1:16:08
  could be tens of thousands, maybe more. They form whenever
• 1:16:13
  a sufficiently massive star collapses with the right properties. Given
• 1:16:19
  how many massive stars exist, magnetar formation should be relatively common,
• 1:16:26
  which means the universe contains countless stellar objects with magnetic
• 1:16:31
  fields strong enough to distort atoms and alter the properties
• 1:16:35
  of space time itself. Most of them sit quietly, slowly
• 1:16:40
  radiating away their magnetic energy over ten thousand years. Occasionally
• 1:16:46
  one cracks, releasing a burst of gamma rays that briefly
• 1:16:50
  outshines entire galaxies. Then it fades back into relative obscurity.
• 1:16:56
  This is the pattern we keep seeing. Power in the
• 1:16:59
  universe concentrates, black holes, accrete, magnetic fields amplify, stars explode,
• 1:17:07
  but these events are temporary or localized. The universe as
• 1:17:11
  a whole remains relatively calm. Most of space is empty.
• 1:17:16
  Most of time passes without drama, but when energy does
• 1:17:20
  concentrate when conditions aligne the results are spectacular. Magnetars also
• 1:17:27
  connect to another class of extreme events. When two neutron
• 1:17:31
  stars orbit each other, they gradually spiral inward, losing energy
• 1:17:36
  to gravitational waves. Eventually they merge. The collision releases a
• 1:17:42
  killer nova, an explosion about a thousand times brighter than
• 1:17:46
  a classical nova. The merger also produces a gamma ray burst,
• 1:17:51
  typically a short one lasting a few seconds, and it
• 1:17:54
  creates heavy elements. Neutron rich matter ejected during the collision
• 1:18:00
  undergoes rapid neutron capture. Elements beyond iron form in this process, gold, platinum, uranium,
• 1:18:09
  the iodine in your thyroid, the gold in any jewelry
• 1:18:13
  you own. Most of the heaviest elements on Earth came
• 1:18:17
  from neutron star mergers billions of years ago, before the
• 1:18:22
  Solar system formed. The August twenty seventeen detection of gravitational
• 1:18:28
  waves from merging neutron stars confirmed this. Lego and Virgo
• 1:18:34
  detected the gravitational signal. Telescopes around the world observed the
• 1:18:40
  Keelan over spectroscopy of the explosion showed signatures of heavy
• 1:18:45
  element formation for the first time. We watch the universe
• 1:18:49
  create gold in real time, well, real time delayed by
• 1:18:54
  one hundred and thirty million years. The merger happened in
• 1:18:58
  a galaxy called n g C four nine nine three.
• 1:19:03
  The light and gravitational waves traveled for one hundred and
• 1:19:07
  thirty million years before reaching Earth, but when they arrived,
• 1:19:12
  we caught them, We measured them, we learned. The power
• 1:19:17
  released in that final second before merger is staggering. Two
• 1:19:22
  neutron stars, each about one point four solar masses, spiraling
• 1:19:27
  together at a significant fraction of light speed. The gravitational
• 1:19:32
  waves they emit carry away energy. In the last second,
• 1:19:38
  they radiate more power than all the stars in the
• 1:19:41
  visible universe combined. Let that settle for a moment. All
• 1:19:46
  the stars in the observable universe hundreds of billions of galaxies,
• 1:19:51
  each containing hundreds of billions of stars fusing hydrogen radiating light.
• 1:19:58
  The combined output is an enormous, but in the final
• 1:20:02
  second before two neutron stars merge, their gravitational wave emission
• 1:20:08
  exceeds that combine stellar output by orders of magnitude. This
• 1:20:13
  is power on a scale that makes stellar fusion look insignificant,
• 1:20:19
  and it happens in a region of space smaller than
• 1:20:22
  a city. The densities involved are beyond extreme. The energies
• 1:20:28
  are incomprehensible. The physics pushes against the limits of general relativity.
• 1:20:35
  After the merger. What's left sometimes another neutron star more
• 1:20:41
  massive than either progenitor, sometimes a black hole. Depends on
• 1:20:47
  the total mass. If the remnant exceeds about two point
• 1:20:51
  five solar masses, collapse to a black hole is inevitable.
• 1:20:57
  Nothing can support that much mass in such a small volume.
• 1:21:01
  If a massive neutron star forms, it might be a magnetar.
• 1:21:06
  The magnetic fields from both progenitor stars twisted and amplified
• 1:21:11
  during the merger, could produce a field even stronger than
• 1:21:14
  normal magnetars. These merger remnants might be the strongest magnets
• 1:21:19
  in the universe. We haven't confirmed this directly. The objects
• 1:21:25
  are distant the after glows fade quickly, but the theoretical
• 1:21:30
  models suggest its possible may be even likely, which means
• 1:21:35
  some of the magnetars we observe today could be merger
• 1:21:39
  remnants neutron stars that came from the collision of two
• 1:21:44
  other neutron stars, the universe recycles its extremes. This brings
• 1:21:50
  us back to a central theme. The most powerful objects
• 1:21:54
  and events in the universe are connected. Massive stars create
• 1:21:59
  neutron stars and black holes. Neutron stars merge, creating heavy
• 1:22:05
  elements and possibly more neutron stars. Black Holes accrete, launching
• 1:22:12
  jets that shape galaxies. Galaxies collide, funneling gas into their
• 1:22:17
  central black holes, igniting quasars. It's a cycle, not a
• 1:22:23
  perfect loop, but a network of cause and effect spanning
• 1:22:27
  cosmic time scales. The power we observe today came from
• 1:22:32
  processes that began billions of years ago. The explosions we
• 1:22:36
  detect across the universe are consequences of stellar evolution, of
• 1:22:41
  gravitational dynamics, of quantum mechanics operating under extreme conditions, and
• 1:22:47
  all of it follows from the same basic physics general relativity, thermodynamics, electromagnetism,
• 1:22:56
  the strong and weak nuclear forces. No new laws needed,
• 1:23:01
  just the same principles we test in laboratories, applied to
• 1:23:05
  regimes where gravity is strong, densities are extreme, and energies
• 1:23:10
  reach levels we can barely produce in colliders. The universe
• 1:23:15
  is consistent. The laws don't change based on scale. A
• 1:23:20
  magneta's field follows Maxwell's equations, a neutron star merger follows
• 1:23:25
  Einstein's field equations. The particle acceleration in a blazer jet
• 1:23:30
  follows the Lawrence force law. We can describe it all
• 1:23:34
  with mathematics developed on Earth, tested in controlled environments, extended
• 1:23:41
  to cosmic extremes. That's worth appreciating. The most powerful objects
• 1:23:47
  in the universe aren't mysterious. In principle. We understand the physics,
• 1:23:53
  We can calculate the energies, we can predict the outcomes.
• 1:23:58
  The challenge isn't the physics, it's the scale. A magnetar's
• 1:24:03
  field is strong, but we know how magnetic fields work.
• 1:24:08
  A gamma ray burst is energetic, but we know how
• 1:24:11
  shock waves accelerate particles. A quasar is luminous, but we
• 1:24:17
  know how accretion discs radiate. The mechanisms are known, the
• 1:24:22
  equations are solved, the mystery is gone. What remains is ore,
• 1:24:28
  because understanding something doesn't make it less impressive. Knowing how
• 1:24:33
  a magnetar generates its field doesn't reduce the fact that
• 1:24:37
  it's a quadrillion time stronger than Earth's. Calculating the energy
• 1:24:42
  output of a quasar doesn't change that it outshines a
• 1:24:46
  trillion stars. Measuring a gamma ray burst doesn't diminish the
• 1:24:51
  fact that it releases more energy in seconds than the
• 1:24:55
  Sun will in its entire lifetime. The numbers speak for themselves,
• 1:25:01
  and the numbers are extraordinary, and they define what's possible
• 1:25:06
  in the universe. Now you're probably wondering something. If black
• 1:25:11
  holes and their jets dominate the power rankings, what about
• 1:25:16
  other extreme objects? What about the densest stars? What about
• 1:25:22
  magnetic fields so strong they warp the fabric of reality itself?
• 1:25:27
  Enter magnetars. Magnetars are neutron stars, but calling them that
• 1:25:32
  is like calling a supernova a bright light. There neutron
• 1:25:37
  stars with magnetic fields so powerful they redefine what we
• 1:25:41
  mean by strong. A typical neutron star has a magnetic
• 1:25:46
  field about a trillion times stronger than Earth's, already absurd,
• 1:25:51
  already beyond human scale. A magnetar multiplies that by another thousand.
• 1:25:58
  The numbers become almost meaningless. A magnetar's magnetic field reaches
• 1:26:04
  ten to the fourteenth Gauss, sometimes ten to the fifteenth.
• 1:26:09
  That's a quadrillion times stronger. Than Earth's field. The strongest
• 1:26:15
  magnetic field humans have ever created in a laboratory peaks
• 1:26:19
  around a million gauss. A magneta's field is one hundred
• 1:26:25
  million times stronger than that. What does a field like
• 1:26:29
  that actually do? It distorts atoms. Hydrogen, the simplest element,
• 1:26:36
  gets compressed to a fraction of its normal width. The
• 1:26:40
  electron orbits stretch and deform under the magnetic stress. Chemistry
• 1:26:45
  as we know it stops working. At a distance of
• 1:26:49
  a thousand kilometers, a magnetar's field would be lethal, not
• 1:26:54
  because of radiation, though there's plenty of that, because the
• 1:26:58
  magnetic field its would tear apart the electron clouds in
• 1:27:03
  your atoms. The biochemistry that keeps you alive would simply
• 1:27:08
  cease to function. Closer in, things get stranger. The magnetic
• 1:27:13
  field becomes so intense it affects the vacuum of space.
• 1:27:18
  Empty space under normal conditions is isotropic. Light travels the
• 1:27:24
  same speed in all directions, but near a magneta, the
• 1:27:28
  vacuum becomes biafringent. Light polarized in different directions, travels at
• 1:27:33
  different speeds. Space itself develops properties we normally associate with crystals.
• 1:27:41
  This isn't theoretical. We've measured it. The power output of
• 1:27:45
  a magnetar doesn't come from fusion. Neutron stars don't fuse anything,
• 1:27:51
  their cores are too dense. Instead, magnetars get their energy
• 1:27:56
  from their magnetic fields. As the field decay over thousands
• 1:28:01
  of years, it releases energy. The star's crust under immense
• 1:28:06
  strain from the shifting field lines occasionally cracks. These are
• 1:28:12
  called starquakes. The name sounds almost gentle, it's not a
• 1:28:18
  typical starquake on a magnetar releases more energy in a
• 1:28:22
  fraction of a second than the Sun produces in one
• 1:28:24
  hundred thousand years. That's ten to the forty sixth ergs.
• 1:28:31
  To put that in perspective, if you could somehow convert
• 1:28:34
  a single kilogram of matter entirely into energy, you'd get
• 1:28:39
  about ten to the twenty first ergs. A magnetar starquake
• 1:28:45
  releases energy equivalent to converting ten billion trillion kilograms of
• 1:28:50
  matter into pure radiation in the tenth of a second.
• 1:28:55
  December twenty seventh, two thousand and four, a magnetar called
• 1:28:59
  s s GR one eight zero six DASH two zero
• 1:29:03
  had one of these outbursts. The gamma ray pulse was
• 1:29:07
  so intense its saturated detectors on satellites designed specifically to
• 1:29:11
  measure gamma ray bursts. The pulse traveled fifty thousand light
• 1:29:17
  years across the galaxy. When it hit Earth's upper atmosphere,
• 1:29:22
  it partially ionized the ionosphere. From halfway across the Milky Way,
• 1:29:27
  a stellar object the size of a city temporarily disrupted
• 1:29:32
  our planet's atmospheric chemistry. If that magnetar had been ten
• 1:29:37
  light years away instead of fifty thousand, the burst would
• 1:29:42
  have triggered a mass extinction. Magnetars exist because of how
• 1:29:47
  neutron stars form. When a massive star collapses, conservation of
• 1:29:52
  angular momentum spins up the core. Conservation of magnetic flux
• 1:29:58
  amplifies the field. If the original star had even a
• 1:30:02
  modest magnetic field, the collapse concentrates it. The field lines
• 1:30:08
  frozen into the stellar material compress along with everything else.
• 1:30:12
  The result is a star twenty kilometers across with a
• 1:30:16
  mass one point four times the sun. The density is
• 1:30:20
  so extreme that a teaspoon of neutron star material would
• 1:30:24
  weigh a hundred million tons on Earth. The magnetic field
• 1:30:28
  threading through this ultra dense matter reaches levels that simply
• 1:30:33
  don't exist anywhere else in nature. The field energy alone
• 1:30:38
  contributes measurably to the star's gravitational mass. But here's what
• 1:30:44
  makes magnetars particularly interesting for our discussion about power. They're
• 1:30:50
  not the most luminous objects. Quasers outshine them by enormous margins.
• 1:30:57
  They're not the most energetic events. Gamma ray bursts release
• 1:31:02
  more total energy. But magnetars have the strongest magnetic fields
• 1:31:07
  ever measured in the universe, and magnetic fields are a
• 1:31:11
  form of power. They can accelerate particles, they can store energy,
• 1:31:17
  They can do work across vast distances. A magnetar sitting
• 1:31:21
  in empty space doesn't just radiate, It creates a magnetosphere
• 1:31:27
  extending thousands of kilometers outward. Any charged particle entering that
• 1:31:32
  region gets accelerated to relativistic speeds. The field lines twist
• 1:31:38
  and snap, releasing bursts of X rays and gamma rays.
• 1:31:43
  The star essentially becomes a particle accelerator, operating continuously for millennia.
• 1:31:50
  This matters for how we think about power distribution in
• 1:31:53
  the universe. Quasers and blazers represent one mode accretion on
• 1:32:00
  to supermassive black holes, converting gravitational potential energy into radiation
• 1:32:07
  and kinetic energy of jets. Gamma ray bursts represent another
• 1:32:14
  explosive events, releasing stored energy all at once. Magnetars represent
• 1:32:20
  a third mode, sustained power from magnetic field decay. It's
• 1:32:25
  a different mechanism entirely, no accretion disk, no jet, just
• 1:32:30
  a magnetic field so strong it dominates the local environment
• 1:32:34
  and radiates energy as it slowly unwinds. And here's something
• 1:32:39
  you might not expect. Magnetars probably aren't that rare. We've
• 1:32:45
  found about thirty confirmed magnetars in the Milky Way, but
• 1:32:49
  our galaxy is big and magnetars are hard to detect
• 1:32:53
  unless they're actively flaring. The estimated population could be tens
• 1:32:58
  of thousands. Maybe they form whenever a sufficiently massive star
• 1:33:03
  collapses with the right properties. Given how many massive stars exist,
• 1:33:10
  magnetar formation should be relatively common, which means the universe
• 1:33:16
  contains countless stellar objects with magnetic fields strong enough to
• 1:33:21
  distort atoms and alter the properties of space time itself.
• 1:33:26
  Most of them sit quietly, slowly radiating away their magnetic
• 1:33:31
  energy over ten thousand years. Occasionally one cracks releasing a
• 1:33:37
  burst of gamma rays that briefly outshines entire galaxies, then
• 1:33:42
  it fades back into relative obscurity. This is the pattern
• 1:33:46
  we keep seeing. Power in the universe concentrates, black holes, accrete,
• 1:33:52
  magnetic fields amplify, stars explode, but these events are temporary
• 1:33:58
  or localized. The universe as a whole remains relatively calm.
• 1:34:03
  Most of space is empty, most of time passes without drama,
• 1:34:08
  but when energy does concentrate when conditions are line, the
• 1:34:13
  results are spectacular. Magnetures also connect to another class of
• 1:34:18
  extreme events. When two neutron stars orbit each other, they
• 1:34:23
  gradually spiral inward, losing energy to gravitational waves. Eventually they merge.
• 1:34:31
  The collision releases a kilo nova, an explosion about a
• 1:34:35
  thousand times brighter than a classical nova. The merger also
• 1:34:40
  produces a gamma ray burst, typically a short one lasting
• 1:34:44
  a few seconds, and it creates heavy elements. Neutron rich
• 1:34:50
  matter ejected during the collision undergoes rapid neutron capture. Elements
• 1:34:55
  beyond iron form in this process, gold, platinum, uranium, the
• 1:35:01
  iodine in your thyroid, the gold in any jewelry you own.
• 1:35:07
  Most of the heaviest elements on Earth came from neutron
• 1:35:10
  star mergers billions of years ago, before the Solar system formed.
• 1:35:16
  The August twenty seventeen detection of gravitational waves from merging
• 1:35:20
  neutron stars confirmed this. Ligo and Virgo detected the gravitational signal.
• 1:35:28
  Telescopes around the world observed the Kilanova Spectroscopy of the
• 1:35:32
  explosion showed signatures of heavy element formation. For the first time,
• 1:35:38
  we watched the universe create gold in real time, well,
• 1:35:42
  real time delayed by one hundred and thirty million years.
• 1:35:47
  The merger happened in a galaxy called en GC four
• 1:35:51
  nine nine three. The light and gravitational waves traveled for
• 1:35:56
  one hundred and thirty million years before reaching Earth, but
• 1:36:00
  when they arrived, we caught them. We measured them. We learned.
• 1:36:06
  The power released in that final second before merger is staggering.
• 1:36:11
  Two neutron stars each about one point four solar masses,
• 1:36:16
  spiraling together at a significant fraction of light speed. The
• 1:36:21
  gravitational waves they emit carry away energy. In the last second,
• 1:36:27
  they radiate more power than all the stars in the
• 1:36:30
  visible universe combined. Let that settle for a moment, all
• 1:36:35
  the stars in the observable universe, hundreds of billions of galaxies,
• 1:36:41
  each containing hundreds of billions of stars fusing hydrogen radiating light.
• 1:36:48
  The combined output is enormous, but in the final second
• 1:36:52
  before two neutron stars merge, their gravitational wave emission exceeds
• 1:36:57
  that combined stellar output by orders of magnitude. This is
• 1:37:03
  power on a scale that makes stellar fusion look insignificant,
• 1:37:08
  and it happens in a region of space smaller than
• 1:37:11
  a city. The densities involved are beyond extreme, the energies
• 1:37:17
  are incomprehensible. The physics pushes against the limits of general relativity.
• 1:37:24
  After the merger. What's left sometimes another neutron star more
• 1:37:30
  massive than either progenitor, sometimes a black hole depends on
• 1:37:36
  the total mass. If the remnant exceeds about two point
• 1:37:41
  five solar masses, collapse to a black hole is inevitable.
• 1:37:46
  Nothing can support that much mass in such a small volume.
• 1:37:50
  If a massive neutron star forms, it might be a magnetar.
• 1:37:55
  The magnetic fields from both progenitor stars twisted and amplified
• 1:37:59
  Rura the merger could produce a field even stronger than
• 1:38:03
  normal magnetars. These merger remnants might be the strongest magnets
• 1:38:09
  in the universe. We haven't confirmed this directly, the objects
• 1:38:13
  are distant, the after glows fade quickly, but the theoretical
• 1:38:18
  models suggest it's possible, maybe even likely, which means some
• 1:38:23
  of the magnetars we observe today could be merger remnants
• 1:38:28
  neutron stars that came from the collision of two other
• 1:38:31
  neutron stars. The universe recycles its extremes. This brings us
• 1:38:37
  back to a central theme. The most powerful objects and
• 1:38:40
  events in the universe are connected. Massive stars create neutron
• 1:38:46
  stars and black holes. Neutron stars merge, creating heavy elements
• 1:38:52
  and possibly more neutron stars. Black holes are crete launching
• 1:38:57
  jets that shape galaxies. Galaxies collide, funneling gas into their
• 1:39:04
  central black holes, igniting quasars. It's a cycle, not a
• 1:39:09
  perfect loop, but a network of cause and effect spanning
• 1:39:13
  cosmic time scales. The power we observe today came from
• 1:39:17
  processes that began billions of years ago. The explosions we
• 1:39:22
  detect across the universe are consequences of stellar evolution, of
• 1:39:27
  gravitational dynamics, of quantum mechanics operating under extreme conditions, and
• 1:39:34
  All of it follows from the same basic physics general relativity, thermodynamics, electromagnetism,
• 1:39:42
  the strong and weak nuclear forces. No new laws needed,
• 1:39:47
  just the same principles we test in laboratories, applied to
• 1:39:51
  regimes where gravity is strong, densities are extreme, and energies
• 1:39:57
  reach levels we can barely produce colliders. The universe is consistent.
• 1:40:03
  The laws don't change based on scale. A magnetar's field
• 1:40:08
  follows Maxwell's equations, a neutron star merger follows Einstein's field equations.
• 1:40:16
  The particle acceleration in a blazer jet follows the Lawrenz
• 1:40:20
  force law. We can describe it all with mathematics developed
• 1:40:24
  on Earth, tested in controlled environments, extended to cosmic extremes.
• 1:40:31
  That's worth appreciating. The most powerful objects in the universe
• 1:40:36
  aren't mysterious. In principle. We understand the physics, we can
• 1:40:42
  calculate the energies, we can predict the outcomes. The challenge
• 1:40:47
  isn't the physics, it's the scale. A magneta's field is strong,
• 1:40:53
  but we know how magnetic fields work. A gamma ray
• 1:40:57
  burst is energetic, but we know how or shock waves
• 1:41:01
  accelerate particles. A quasar is luminous, but we know how
• 1:41:06
  accretion discs radiate. The mechanisms are known, the equations are solved,
• 1:41:12
  the mystery is gone. What remains is ow, because understanding
• 1:41:18
  something doesn't make it less impressive. Knowing how a magnetar
• 1:41:23
  generates its field doesn't reduce the fact that its aquadrillion
• 1:41:26
  times stronger than Earth's. Calculating the energy output of a
• 1:41:31
  quasar doesn't change that it outshines a trillion stars. Measuring
• 1:41:37
  a gamma ray burst doesn't diminish the fact that it
• 1:41:40
  releases more energy in seconds than the Sun will in
• 1:41:44
  its entire lifetime. The numbers speak for themselves, and the
• 1:41:50
  numbers are extraordinary. The universe doesn't just produce powerful objects,
• 1:41:56
  It produces observers capable of measuring them. That's the real miracle.
• 1:42:02
  Every instrument we've built, every detector we've launched, every telescope
• 1:42:08
  we've aimed at the sky, is a product of stellar nucleosynthesis.
• 1:42:13
  The silicon in our chips, the aluminum in our spacecraft,
• 1:42:17
  the gold in our connectors all forged in stellar cores
• 1:42:21
  or neutron star mergers. We're using the products of cosmic
• 1:42:26
  violence to study cosmic violence. That feedback loop is profound.
• 1:42:32
  The universe created the elements necessary for complex chemistry. Complex
• 1:42:37
  chemistry produced life, life, evolved, intelligence, intelligence developed technology. Technology
• 1:42:47
  measures the processes that created the technology. We're inside the system.
• 1:42:51
  We're studying, not external observers, but participants. The atoms in
• 1:42:58
  your brain contemplating magnetars were once inside stars. The calcium
• 1:43:04
  in your bones clicking a mouse to view gamma ray
• 1:43:07
  burst data came from supernova explosions. You're not separate from
• 1:43:13
  these cosmic phenomena, You're made of them. This changes the
• 1:43:19
  nature of the question. We're not asking what's the most
• 1:43:23
  powerful object in the universe from outside, We're asking it
• 1:43:27
  from within as arrangements of atoms that once participated in
• 1:43:33
  these very processes. That perspective matters because power isn't just
• 1:43:39
  about energy output. It's about consequences, about impact, about what
• 1:43:47
  changes because the object exists. A gamma ray burst releases
• 1:43:51
  extraordinary energy, but it's brief seconds or minutes. Then it's
• 1:43:58
  Overdiation propagates outward at light speed, thinning as it expands.
• 1:44:05
  After a few thousand years, it's undetectable. A magnetar maintains
• 1:44:10
  its field for thousands of years, maybe millions. The energy
• 1:44:15
  isn't released in one burst, but sustained over geological time scales.
• 1:44:20
  Different kind of power, same fundamental physics. A quasar shines
• 1:44:26
  for millions or billions of years, steady, relentless output, not
• 1:44:33
  the brief spike of a gamma ray burst, but sustained
• 1:44:36
  luminosity that shapes galactic evolution. The radiation pressure from a
• 1:44:41
  quasar can shut down star formation across an entire galaxy.
• 1:44:47
  It can drive gas out of the galactic core, starving
• 1:44:51
  the central black hole, eventually shutting itself off. That's negative feedback.
• 1:44:57
  The quasar's power regulates its own fuel supply. Too much output,
• 1:45:02
  too much radiation pressure, gas gets expelled, accretion rate drops,
• 1:45:08
  luminosity decreases, equilibrium. The universe self regulates even at these extremes.
• 1:45:16
  Black hole merges are different again, singular events, two massive
• 1:45:21
  objects spiraling together over millions of years, then merging in seconds.
• 1:45:28
  The gravitational wave output during that final merger exceeds the
• 1:45:33
  electromagnetic luminosity of all stars in the observable universe, but
• 1:45:39
  only for a fraction of a second, which is more
• 1:45:42
  powerful the brief, but incomprehensible spike or the sustained output
• 1:45:49
  over cosmic time scales. The answer depends on what you're measuring.
• 1:45:53
  Peak luminosity favors the merger. Total energy output might favor
• 1:45:58
  the quasar. Impact on surrounding environment could go either way.
• 1:46:04
  There's no single metric that captures power completely. We can
• 1:46:08
  measure energy per second, energy per unit, mass, energy per
• 1:46:14
  unit volume, magnetic field strength, gravitational potential. Each metric gives
• 1:46:22
  a different answer. Magnetars win on magnetic field strength, nothing
• 1:46:27
  else comes close, but their total energy output is lower
• 1:46:31
  than quasars. Quasars win on sustained luminosity, but their peak
• 1:46:37
  output is lower than gamma ray bursts. Gamma ray bursts
• 1:46:42
  win on brief luminosity, but their total lifetime energy is
• 1:46:46
  less than a quasars black hole. Mergers win on gravitational
• 1:46:51
  wave output, but that's a different kind of radiation, not electromagnetic,
• 1:46:57
  not directly observable until re The Offyucus supercluster eruption released
• 1:47:04
  more total energy than any gamma ray burst by a
• 1:47:09
  factor of millions, but it took one hundred million years.
• 1:47:15
  The energy was spread out over time, less intense, more sustained,
• 1:47:21
  So the question fragments. Most powerful becomes most powerful at
• 1:47:25
  what most luminous, most energetic, per second, most total energy,
• 1:47:32
  strongest field, deepest gravitational. Well, each has a different answer,
• 1:47:38
  and each answer is correct within its context. But there's
• 1:47:42
  another angle, power relative to size. Quasars emit incredible luminosity
• 1:47:49
  from a region the size of the Solar system. That's compact,
• 1:47:54
  But neutron stars pack similar mass into a sphere twenty
• 1:47:58
  kilometers across. That's density. That's concentration. A black hole's event
• 1:48:04
  horizon is smaller. Still, all the mass compressed to a
• 1:48:08
  point classically quantum gravity probably prevents a true singularity, but
• 1:48:14
  the scale is still subatomic. Everything inside the event horizon,
• 1:48:20
  all the information, all the mass, all the angular momentum
• 1:48:26
  contained within a boundary measured in kilometers for stellar mass
• 1:48:29
  black holes or solar system scales for supermassive ones. That
• 1:48:35
  concentration of spacetime curvature is extreme. Nothing curves spacetime more severely.
• 1:48:43
  The gradient near the event horizon is the steepest possible
• 1:48:47
  without creating a naked singularity, which the cosmic censorship hypothesis
• 1:48:53
  suggests doesn't happen. So black holes might win on spacetime curvature,
• 1:48:59
  magnetars on field strength, quasas on sustained luminosity, gamma ray
• 1:49:05
  bursts on peak electromagnetic output, black hole mergers, on gravitational
• 1:49:10
  wave luminosity. No single winner, just different categories of extreme,
• 1:49:16
  and all of it observable, detectable, measurable. We've built instruments
• 1:49:23
  sensitive enough to detect these phenomena across billions of light years.
• 1:49:28
  Gravitational wave detectors that measure distortions smaller than the width
• 1:49:32
  of a proton X ray, telescopes that resolve emission from
• 1:49:37
  accretion disks around black holes, radio arrays that image jets
• 1:49:42
  from quasars. The technology required to observe these objects is
• 1:49:46
  itself remarkable. Intoferometry, adaptive optics, space based detectors above the atmosphere,
• 1:49:55
  cryogenic sensors cooled to millikelvin temperatures. We've constructed machines that
• 1:50:02
  operate at the quantum limit of measurement, gravitational wave detectors
• 1:50:08
  limited by quantum fluctuations in their mirrors, radio receivers cooled
• 1:50:14
  until thermal noise is minimized, fote on counters that register
• 1:50:19
  individual gamma rays. The engineering required to detect the universe's
• 1:50:24
  most powerful objects pushes our technology to fundamental limits, limits
• 1:50:29
  set by quantum mechanics, by thermodynamics, by the speed of light.
• 1:50:35
  We can't measure gravitational waves more precisely without confronting quantum uncertainty.
• 1:50:41
  We can't detect fainter sources without longer integration times or
• 1:50:47
  larger collectors. We can't resolve smaller angular scales without bigger
• 1:50:53
  baselines or shorter wave lengths. Every observation bumps against physical limits,
• 1:51:00
  but we keep finding ways to push those limits further.
• 1:51:04
  Better mirrors, larger arrays, more sensitive detectors, clever analysis techniques
• 1:51:11
  that extract signal from noise, and every improvement reveals more
• 1:51:17
  more distant quasars, more gamma ray bursts, more neutron star mergers,
• 1:51:23
  more magnetars. The universe keeps providing examples, we keep finding them.
• 1:51:30
  The detection rate increases with our sensitivity, which means there's
• 1:51:35
  more out there, fainter objects, more distant events phenomena we
• 1:51:41
  haven't yet characterized. Every survey finds outliers, objects that don't
• 1:51:46
  fit the models, too luminous, too compact, two variable. These
• 1:51:52
  outliers drive theory forward force refinements reveal new physics. GRB
• 1:51:58
  two two one zero zero zero nine A was an
• 1:52:01
  outlier brightest ever detected its saturated detectors designed for brighter vents.
• 1:52:08
  We had to use indirect methods to measure its peak flux,
• 1:52:12
  too bright for direct observation. That happens. The universe occasionally
• 1:52:18
  produces something so extreme it breaks our instruments. Not because
• 1:52:23
  the instruments are poorly designed. They're built for the typical case,
• 1:52:28
  the statistical average, but the universe has a tail extreme
• 1:52:34
  events that occur rarely but do occur. We design for
• 1:52:39
  the expected. Then nature surprises us and we learn upgrade
• 1:52:45
  the detectors, expand the dynamic range, build backups with different sensitivities.
• 1:52:52
  The next generation of instruments will handle brighter bursts, wider fields,
• 1:52:58
  higher time resolution. They'll find more events, rarer phenomena, and
• 1:53:04
  some of those will be outliers for the new instruments.
• 1:53:08
  It's iterative. Each generation of detectors reveals a new population,
• 1:53:13
  which informs the next generation, which finds more. The process continues,
• 1:53:19
  but there are hard limits cosmological limits. We can't see
• 1:53:25
  past the cosmic horizon. Light from beyond that distance hasn't
• 1:53:29
  reached us yet. As the universe expands, that horizon grows,
• 1:53:35
  but it grows at the speed of light, which means
• 1:53:39
  distant objects recede faster than their light can reach us.
• 1:53:44
  There's a sphere of observability. Everything inside is potentially detectable,
• 1:53:51
  everything outside is forever beyond our reach. That sphere has
• 1:53:55
  a finite volume, which means a finite number of objects.
• 1:54:01
  We can count them statistically. We can't observe every galaxy,
• 1:54:07
  but we can survey representative volumes and extrapolate. Current estimates
• 1:54:14
  suggest around two trillion galaxies in the observable universe. Each
• 1:54:20
  galaxy has a supermassive black hole. Most are dormant, some
• 1:54:25
  are active. A small fraction are quasars. An even smaller
• 1:54:30
  fraction are the brightest quasars. The extreme tail of the
• 1:54:35
  luminosity distribution. We can calculate the number of magnetars, the
• 1:54:40
  supernova rate, the fraction that produced neutron stars, the fraction
• 1:54:46
  of neutron stars that are magnetars. Multiply the probabilities get
• 1:54:51
  an estimate. Gamma ray bursts are rarer a few per
• 1:54:56
  galaxy per million years. Multiply by two trillion galls lexies.
• 1:55:01
  Divide by the observable time scale, get a rate. Compare
• 1:55:06
  to detection rates. The numbers match. That's consistency the model's work.
• 1:55:13
  The statistics are correct. We understand the populations, not every
• 1:55:18
  individual object, but the ensemble, the distribution, the average properties,
• 1:55:25
  which brings us back to power. The most powerful individual
• 1:55:29
  object is probably an outlier, something rare, but rare doesn't
• 1:55:34
  mean nonexistent. The universe is large. Outliers exist, we just
• 1:55:41
  haven't found all of them yet. The brightest quasar we've
• 1:55:45
  detected might not be the brightest that exists, just the
• 1:55:49
  brightest we've seen. There could be brighter ones beyond our
• 1:55:53
  detection limit, or pointed away from us, or obscured by dust.
• 1:55:59
  Same for ge gamma ray bursts, same for magnetars, same
• 1:56:04
  for everything. Our catalogs are incomplete, biased toward bright nearby,
• 1:56:11
  unobscured sources. The true maximum might be larger. The true
• 1:56:16
  distribution might extend further. We're sampling the observable subset, not
• 1:56:23
  the complete population, but we can estimate, extrapolate, use the
• 1:56:28
  observed distribution to predict the unobserved tail. Statistical methods Bayesian inference,
• 1:56:35
  maximum likelihood those methods suggest the brightest quasers we've found
• 1:56:41
  are probably within a factor of a few of the
• 1:56:44
  absolute maximum. Same for gamma ray bursts. The outliers are
• 1:56:49
  rare enough that we've likely found representatives near the extreme.
• 1:56:53
  Magnetars are harder, smaller sample size, more difficult to detect.
• 1:56:59
  The strongest fields we've measured might be average, or we
• 1:57:03
  might have found the extreme cases. Uncertainty remains. Black holes
• 1:57:08
  scale with galaxy mass. The most massive galaxies host the
• 1:57:12
  most massive black holes. We've found black holes with masses
• 1:57:17
  of tens of billions of solar masses. Could there be
• 1:57:21
  larger ones, probably in the most massive galaxy clusters. We
• 1:57:27
  just haven't surveyed them all yet, But there's a practical maximum.
• 1:57:32
  Galaxy mergers produce larger black holes, but mergers take time.
• 1:57:38
  The universe has a finite age. There's a limit to
• 1:57:42
  how many mergers can occur, which limits the maximum black
• 1:57:46
  hole mass. Current estimates suggest the maximum is around one
• 1:57:52
  hundred billion solar masses, maybe higher, but not arbitrarily high.
• 1:57:58
  The universe isn't old enough for more. That maximum mass
• 1:58:02
  corresponds to a maximum gravitational influence, maximum accretion power, maximum
• 1:58:08
  jet luminosity not infinite, bounded by cosmology, so even the
• 1:58:15
  extremes have limits, physical limits, observational limits, statistical limits. The
• 1:58:22
  most powerful object in the universe is powerful, but not infinitely,
• 1:58:27
  so it operates within the same physical laws as everything else.
• 1:58:33
  Just push to the edge of what those laws allow.
• 1:58:36
  That's the real answer. The universe has extremes, but the
• 1:58:40
  extremes are finite, bounded by physics, by time, by space,
• 1:58:47
  by probability. Understanding those bounds is understanding the universe itself,
• 1:58:53
  which raises an interesting question. If the extremes are bounded
• 1:58:57
  by physics, what determines those start with energy? The most
• 1:59:03
  powerful objects convert mass to energy. Black Holes do this
• 1:59:07
  through accretion matter falls in, heats up radiates. The efficiency
• 1:59:13
  depends on spin. A non rotating black hole converts about
• 1:59:18
  six percent of in falling mass to energy. That's already
• 1:59:22
  better than fusion. Stars convert less than one percent, but
• 1:59:27
  spinning black holes can reach forty two percent efficiency. Nearly
• 1:59:32
  half the mass becomes radiation. That's the theoretical maximum for accretion.
• 1:59:39
  The Euffucus supercluster eruption consumed two hundred seventy million solar
• 1:59:44
  masses over one hundred million years. Most of that mass
• 1:59:48
  went into the black hole, but some became energy jets,
• 1:59:53
  radiation shock waves. The cavity it carved is one point
• 1:59:58
  five million light year across ten times the Milky Way's diameter.
• 2:00:04
  That sustained power not a brief burst, continuous output for
• 2:00:10
  geological time scales compare to gamma ray bursts. They release
• 2:00:16
  more energy in seconds than the Sun will produce in
• 2:00:19
  its entire lifetime, but they're transient brief. The total energy
• 2:00:25
  might be comparable to what a quasar emits in a year,
• 2:00:29
  compressed into moments instead of spread across time. So which
• 2:00:34
  is more powerful, the brief intense burst or the sustained
• 2:00:38
  output depends on your definition. Peak luminosity favors gamma ray bursts,
• 2:00:45
  total energy output favors quasars and active galactic nuclei. It's
• 2:00:51
  like comparing a camera flash to a light bulb. One
• 2:00:54
  is brighter for an instant, the other provides more total
• 2:00:58
  light over time. Magnetars add another dimension. Their power isn't
• 2:01:04
  primarily electromagnetic radiation, its magnetic field strength. The field itself
• 2:01:11
  does work, twists space time, affects particle trajectories at cosmic distances.
• 2:01:18
  A magnetar's magnetic field can warp atoms into elongated shapes,
• 2:01:24
  change the vacuum properties of space itself. That's a different
• 2:01:28
  kind of power. The December two thousand four starquake from
• 2:01:33
  SGR one eight six DASH two oh released more energy
• 2:01:38
  in a fraction of a second than the Sun produces
• 2:01:41
  in one hundred thousand years. But that wasn't continuous output.
• 2:01:46
  It was a crack in the crust, a sudden release.
• 2:01:49
  The magnetar itself maintains its field constantly. That requires energy.
• 2:01:56
  Where does it come from? Rotational energy? Magnetar spin not
• 2:02:01
  as fast as millisecond pulsars, but fast enough. The rotation
• 2:02:06
  powers the magnetic field. As the field does work, the
• 2:02:09
  rotation slows gradually over thousands of years, the rotational energy
• 2:02:16
  gets converted to magnetic energy, which gets released as X
• 2:02:20
  rays and gamma rays. So the power source is kinetic
• 2:02:24
  energy from the original supernova stored in rotation, released slowly
• 2:02:30
  through magnetic processes. It's a cosmic battery charged by stellar collapse,
• 2:02:36
  discharged over millennia. Black holes have a different power source, gravity,
• 2:02:43
  specifically gravitational potential energy. Matter far from a black hole
• 2:02:49
  has high potential energy. As it falls closer, that potential
• 2:02:53
  energy converts to kinetic energy, then to heat, then to radiation.
• 2:03:00
  The deeper the gravitational well, the more energy available per
• 2:03:04
  kilogram of matter. That's why the most massive black holes
• 2:03:09
  can be the most luminous. They have the deepest wells.
• 2:03:14
  Matter falling in can release more energy, but there's a limit,
• 2:03:19
  the Eddington limit. Radiation pressure pushes outward, gravity pulls inward.
• 2:03:26
  When radiation pressure equals gravitational force, accretion stops. No more
• 2:03:32
  matter can fall in. The luminosity is capped. For a
• 2:03:36
  given black hole mass, there's a maximum luminosity Eddington luminosity
• 2:03:42
  proportional to mass. A billion solar mass black hole has
• 2:03:47
  an Eddington luminosity about a billion times the suns. That's
• 2:03:53
  roughly ten to the forty seventh power ergs per second,
• 2:03:57
  which matches the brightest quasers. But some objects exceed the
• 2:04:02
  Eddington limit briefly during special circumstances. Super Eddington accretion happens
• 2:04:09
  when matter falls in so fast that radiation can't escape efficiently.
• 2:04:15
  Gets trapped in the flow allows more matter to accrete,
• 2:04:19
  produces higher luminosities, but it's unstable, can't last long. That
• 2:04:25
  might explain ultra luminous quasars, the ones pushing ten to
• 2:04:30
  the forty eighth power ergs per second. They're temporarily exceeding
• 2:04:35
  their Eddington limit, consuming matter faster than steady state physics allows.
• 2:04:42
  It'll end eventually, the system will stabilize, but for now
• 2:04:49
  they're extraordinarily bright. Gamma ray bursts might also involve super
• 2:04:54
  Eddington processes. The jets definitely do. A relativistic jet carries
• 2:05:00
  enormous energy, more than the Eddington luminosity of the central engine,
• 2:05:06
  but the jet is directional beamed, so it doesn't push
• 2:05:11
  on the surrounding matter the same way isotropic radiation does.
• 2:05:16
  Different geometry, different limits, which brings up blazers. They're quasers
• 2:05:22
  with jets pointed at us. We see the jet head
• 2:05:26
  on that makes them appear brighter relativistic beaming, the light
• 2:05:32
  is compressed, blue shifted, concentrated. A blazer might have the
• 2:05:38
  same intrinsic power as a regular quasar, but we see
• 2:05:42
  it amplified by geometry. Measurements show apparent speeds in blazer
• 2:05:48
  jets exceeding twenty five times the speed of light. That's
• 2:05:53
  not real. Faster than light motion. It's an illusion. The
• 2:05:58
  jet is moving toward us at nearly the speed of
• 2:06:01
  light close to our line of sight. The light emitted
• 2:06:05
  at different times arrives at Earth within short intervals makes
• 2:06:10
  it look like the jet is moving faster than it
• 2:06:13
  actually is. The true speed is around ninety nine percent
• 2:06:17
  of light speed, still insanely fast at those velocities. Relativistic
• 2:06:25
  effects dominate time dilation, length contraction, Doppler boosting. The energy
• 2:06:33
  we measure is dramatically enhanced compared to what a stationary
• 2:06:37
  observer would see. So blazers aren't necessarily more powerful than
• 2:06:42
  other quasars. They're just pointed at us, Which raises a
• 2:06:47
  question how many powerful objects are out there that we
• 2:06:51
  can't see because they're pointed away from us. For every
• 2:06:55
  blazzer we detect, there might be hundreds of similar objects
• 2:06:59
  with jets aimed elsewhere. We only see the ones aligned
• 2:07:03
  with Earth. That means the total population of jet producing
• 2:07:08
  black holes is much larger than the blazer count suggests.
• 2:07:13
  Same logic applies to gamma ray bursts. We see the
• 2:07:17
  ones with jets pointed at us, but the jets have
• 2:07:20
  narrow opening angles, maybe five to twenty degrees. That means
• 2:07:26
  for every GRB we detect, there are dozens or hundreds
• 2:07:30
  happening with jets pointed in other directions. We miss them entirely.
• 2:07:36
  The true rate of these events is higher than the
• 2:07:39
  observed rate. Multiply by the geometric correction factor, account for
• 2:07:45
  the beaming, get the actual rate that affects our understanding
• 2:07:50
  of how common these extreme objects are. They're rare in
• 2:07:54
  terms of what we detect, but less rare in terms
• 2:07:57
  of what actually occurs. The universe is producing these events constantly,
• 2:08:03
  we just don't see most of them, which means the
• 2:08:06
  most powerful object in the universe might be something we
• 2:08:10
  haven't detected yet, not because it doesn't exist, but because
• 2:08:15
  it's not pointed at us, or it's too far away
• 2:08:20
  or obscured by dust, or in a part of the
• 2:08:23
  sky we haven't surveyed. Current surveys cover a fraction of
• 2:08:28
  the sky at any given time. Overall time, we've covered more,
• 2:08:34
  but not with uniform sensitivity. Deep surveys cover small areas.
• 2:08:38
  Wide surveys are shallower. You can't do both simultaneously with
• 2:08:43
  limited telescope time, so there are gaps regions of parameter
• 2:08:49
  space We haven't explored faint distant objects, transient events that
• 2:08:55
  occurred when no telescope was looking, highly obscured sources that
• 2:09:00
  only show up in infrared or radio wavelengths. We've found some,
• 2:09:04
  but not all. Future telescopes will help. The James Web
• 2:09:09
  Space Telescope is already finding distant quasas that were invisible
• 2:09:13
  to previous instruments. The Vera Ruben Observatory will survey the
• 2:09:19
  entire visible sky every few nights, catching transience, building time
• 2:09:25
  domain astronomy. The square Kilometer Array will detect radio sources
• 2:09:31
  with unprecedented sensitivity. Each new instrument expands the observable universe,
• 2:09:38
  not in distance, necessarily, but in the range of phenomena.
• 2:09:42
  We can detect different wavelengths, different time scales, different sensitivities.
• 2:09:50
  Each one reveals objects that were always there but invisible
• 2:09:54
  to older technology. That means our current answer to most
• 2:09:59
  powerful obs is provisional. It's the most powerful we've found
• 2:10:04
  so far with current instruments in the regions we've surveyed
• 2:10:10
  using the techniques we have, The real most powerful object
• 2:10:14
  might be hiding just beyond our detection threshold, waiting for
• 2:10:18
  the next generation of telescopes. Or the one after that.
• 2:10:23
  But even with perfect instruments, there's a limit. The observable
• 2:10:28
  universe has a finite volume, roughly four times ten to
• 2:10:32
  the eighty cubic meters. That volume contains a finite number
• 2:10:37
  of galaxies, around two trillion. Each galaxy has a finite
• 2:10:42
  number of possible extreme objects. Multiply the probabilities get an
• 2:10:48
  upper bound on the total count. Within that finite population.
• 2:10:53
  There's a most powerful object singular, the one that happens
• 2:10:58
  to be at the extreme of the distribution. It exists
• 2:11:03
  somewhere we just don't know where, could be in a
• 2:11:07
  galaxy cluster we haven't observed, could be at high redshift.
• 2:11:12
  Could have been active billions of years ago and is
• 2:11:15
  now quiescent. We're seeing the universe at a particular moment.
• 2:11:20
  In cosmic time, objects evolve. What's most powerful today might
• 2:11:28
  not have been a billion years ago. What was most
• 2:11:32
  powerful then might be dormant now. Time adds another layer
• 2:11:37
  of complexity. The universe has a history thirteen point eight
• 2:11:42
  billion years. Objects form, evolve, merge, die. The extreme population
• 2:11:50
  changes over time. In the early universe, the first quasars
• 2:11:54
  were forming smaller black holes, lower masses, lower luminosities, but
• 2:12:00
  there were fewer of them. As the universe aged, black
• 2:12:03
  holes merged, grew larger, became more massive, reached higher peak luminosities,
• 2:12:10
  but the gas supply decreased. Fewer galaxy mergers per unit time,
• 2:12:16
  less fuel for accretion, so the number of active quasers decreased.
• 2:12:21
  Today's most luminous quasers might be less luminous than the
• 2:12:25
  peak quasers at redshift two or three, several billion years ago,
• 2:12:31
  when the universe was younger, more gas rich, more active.
• 2:12:36
  We can observe those distant quasers, see them as they were,
• 2:12:41
  but we can't observe the present day versions. The light
• 2:12:45
  hasn't reached us yet, so the most powerful object that
• 2:12:49
  exists right now might not be the most powerful object
• 2:12:53
  we can currently observe. Light travel time creates a delay.
• 2:12:59
  We see the past, not the present. If we could
• 2:13:02
  freeze the universe, take a snapshot at this exact cosmic time,
• 2:13:07
  survey everything simultaneously, we'd find the true current, most powerful object.
• 2:13:13
  But we can't. We're stuck with the light cone, the
• 2:13:17
  past light cone. Everything we see is history. That history
• 2:13:22
  is valuable. It tells us how objects evolve, how populations change,
• 2:13:28
  over time how the universe transitions from one era to another.
• 2:13:33
  But it means most powerful object in the universe is ambiguous.
• 2:13:39
  Do we mean most powerful currently existing or most powerful
• 2:13:43
  we've observed, or most powerful that ever existed? Different questions,
• 2:13:50
  different answers. The most powerful ever might have been an
• 2:13:54
  early super massive black hole accreting at super Eddington rate
• 2:14:00
  in a dense proto galactic environment, consuming gas at phenomenal rates,
• 2:14:06
  producing a quasar brighter than any we see today. It
• 2:14:10
  existed for maybe one hundred million years, then ran out
• 2:14:15
  of fuel, became quiescent. Still exists now as a dormant
• 2:14:19
  black hole, but we remember its active phase. Or maybe
• 2:14:24
  the most powerful ever was a gamma ray burst from
• 2:14:27
  a hyper nova, a star hundreds of times the Sun's
• 2:14:31
  mass possible in the early universe with different metallicity. It collapsed,
• 2:14:38
  formed a black hole, launched jets, produced a GRB brighter
• 2:14:43
  than any modern one, briefly outshone the entire observable universe
• 2:14:49
  at that time, then faded. The black hole remains, but
• 2:14:55
  the burst is long over. We don't know the past incomplete.
• 2:15:01
  The present is unobservable, The future is uncertain. We work
• 2:15:06
  with what We have the observable subset and make inferences
• 2:15:11
  about the rest. But one thing is clear. Whatever the
• 2:15:15
  most powerful object is, it's operating at the edge of
• 2:15:19
  what physics allows, maximum efficiency, optimal conditions, extreme parameters. It's
• 2:15:28
  not violating physical laws, but it's pushing them to their limits.
• 2:15:33
  That's what makes it the most powerful, not just that
• 2:15:36
  it's powerful, but that it's as powerful as anything can
• 2:15:41
  possibly be given the constraints of relativity, thermodynamics, quantum mechanics, gravity,
• 2:15:50
  all the fundamental forces. The most powerful object is the
• 2:15:55
  one that's found the maximum solution to the optimization problem,
• 2:16:00
  and somewhere in the cosmos it exists. But we can search,
• 2:16:05
  we can observe, we can measure, and we can discover
• 2:16:09
  the next record holder. Because the universe is still active,
• 2:16:14
  still evolving. Somewhere right now, a quasar is brightening, a
• 2:16:20
  magnetar is erupting, a gamma ray burst is launching. The
• 2:16:24
  cosmos doesn't stop for our convenience. It continues operating at
• 2:16:29
  scales that dwarf human comprehension. Every second, somewhere in the
• 2:16:34
  observable universe, matter is being converted to energy at near
• 2:16:39
  maximum efficiency. Black holes are feeding stars are exploding, Neutron
• 2:16:46
  stars are colliding. The machinery of cosmic power runs constantly,
• 2:16:52
  without pause, without rest. And here's what makes it fascinating.
• 2:16:58
  We're getting better at finding these obdts. Technology advances, telescopes
• 2:17:03
  improve detection methods, become more sensitive. The James Web Space
• 2:17:08
  Telescope can see further back in time than ever before,
• 2:17:13
  to epochs when the first quasars were forming, when supermassive
• 2:17:18
  black holes were just beginning to grow. Lego and Virgo
• 2:17:23
  detect gravitational waves from neutron star mergers, from black hole coalescence,
• 2:17:30
  from events that would have been invisible just decades ago.
• 2:17:34
  We're expanding our observational capabilities, pushing into new wavelength regimes.
• 2:17:40
  Gamma ray satellites monitor the entire sky, waiting for the
• 2:17:45
  next burst, the next explosion, the next cosmic catastrophe. Radio
• 2:17:51
  telescope arrays scan for transient events. Optical surveys track changing
• 2:17:57
  brightness across millions of objects. We're building a real time
• 2:18:02
  monitoring system for the universe, watching for the most powerful
• 2:18:06
  events as they happen. Consider what's been discovered just in
• 2:18:10
  recent years. J zero five two nine, Dash four three
• 2:18:16
  five one, the fastest growing black hole known, seventeen billion
• 2:18:21
  solar masses, consuming more than a solar mass per day.
• 2:18:26
  It's accretion disc so luminous it outshines five hundred trillion suns.
• 2:18:31
  That's not a typo five hundred trillion from a region
• 2:18:35
  smaller than our solar system. The efficiency is staggering. Matter
• 2:18:40
  falling into the black hole reaches a significant fraction of
• 2:18:44
  light speed. Friction in the accretion disc heats it to
• 2:18:48
  millions of degrees. It glows across the entire electromagnetic spectrum,
• 2:18:54
  X rays, ultraviolet, visible light, infrared, radio wave. Every photon
• 2:19:01
  detector we point at it saturates with signal. And yet
• 2:19:05
  this object is twelve billion light years away. We're seeing
• 2:19:09
  it as it was when the universe was young, one
• 2:19:12
  tenth its current age. Imagine what it's doing now after
• 2:19:18
  twelve billion more years of growth. It might have consumed
• 2:19:22
  an entire galaxy's worth of gas, or it might have
• 2:19:25
  gone quiescent, run out of fuel, become dormant. We won't
• 2:19:31
  know for twelve billion years when the light from its
• 2:19:35
  current state finally reaches us. But that's just one object,
• 2:19:40
  one data point. The surveys continue SDSS Sloane Digital Sky
• 2:19:47
  Survey has cataloged over nine hundred thousand quasars, each one
• 2:19:52
  powered by a supermassive black hole, each one converting mass
• 2:19:56
  to energy at tremendous rates. The distribution tells us about
• 2:20:00
  galaxy evolution, about how structure formed, about when and where
• 2:20:05
  the most extreme conditions occurred. Statistical analysis reveals patterns. Peak
• 2:20:12
  quaser activity occurred at redshift two to three, about ten
• 2:20:17
  billion years ago, when galaxy merger rates were higher, When
• 2:20:21
  gas fractions were larger, The universe was smaller, denser, more
• 2:20:27
  violent collisions were common. Every collision triggered star formation, fed
• 2:20:33
  central black holes created quasars. The cosmic landscape was ablaze
• 2:20:40
  with activity far more than today. Our current epoch is
• 2:20:44
  relatively quiet, sedate. The universe has aged, spread out, cooled down,
• 2:20:51
  yet individual events still reach extraordinary power levels. GRB two
• 2:20:57
  two one zero zero nine a detected October ninth, twenty
• 2:21:02
  twenty two, the brightest gamma ray burst ever recorded. Its
• 2:21:07
  saturated detectors overwhelmed sensors designed for extreme events. The burst
• 2:21:13
  lasted over three hundred seconds five minutes of continuous high
• 2:21:18
  energy radiation from a source two point four billion light
• 2:21:23
  years away. Despite that distance, it was visible in amateur telescopes.
• 2:21:31
  For a brief moment. A stellar explosion half way across
• 2:21:34
  the observable universe could be seen with back yard equipment.
• 2:21:39
  The total energy released approaches incomprehensible numbers, converting multiple solar
• 2:21:46
  masses worth of matter into pure radiation in minutes. The
• 2:21:51
  mechanism a massive star collapsing, forming a black hole, launching
• 2:21:58
  relativistic jets. The jets punch through the stellar envelope, break
• 2:22:03
  free into space, accelerate material to ninety nine point nine
• 2:22:08
  nine percent light speed. When that material collides with surrounding gas,
• 2:22:14
  it produces the gamma ray emission we detect. The beaming
• 2:22:18
  is crucial. The jets are narrow, perhaps a few degrees wide.
• 2:22:24
  We only see the burst because one jet is pointed
• 2:22:27
  almost directly at us. If it were aimed elsewhere, we'd
• 2:22:32
  miss it entirely, which means for every GRB we detect,
• 2:22:37
  hundreds occur in directions we can't observe. The true rate
• 2:22:42
  of these events is much higher than detection rates suggest.
• 2:22:46
  And then there's the Ophiucus supercluster eruption, discovered in twenty
• 2:22:52
  twenty through careful analysis of X ray data. A cavity
• 2:22:57
  in the intra cluster medium a void one point five
• 2:23:01
  million light years across ten times the Milky Ways diameter,
• 2:23:06
  carved out by a supermassive black hole eruption. The central
• 2:23:11
  black hole has a mass of seven billion suns. It
• 2:23:14
  consumed two hundred seventy million solar masses of material over
• 2:23:19
  one hundred million years. The outflow created shock waves, jets,
• 2:23:25
  bubbles of hot plasma. The cavity represents displaced matter gas
• 2:23:31
  pushed aside by the force of the eruption. The energy
• 2:23:35
  required is staggering five point seven million times more than
• 2:23:39
  the most powerful gamma ray burst, but released over a
• 2:23:43
  much longer time scale, sustained power output for millions of centuries.
• 2:23:49
  It's the most energetic event ever detected since the Big Bang,
• 2:23:54
  a testament to what supermassive black holes can do when
• 2:23:58
  properly fed, when conditions align, when accretion rates maximize. These
• 2:24:05
  discoveries reshape our understanding. They push the boundaries of what
• 2:24:09
  we thought possible. Each new detection forces theoretical revisions. Models
• 2:24:16
  must accommodate observations, simulations must reproduce measurements The interplay between
• 2:24:23
  theory and observation drives progress. We predict, we observe, we refine,
• 2:24:31
  we predict again. The cycle continues. Our picture of cosmic
• 2:24:36
  power becomes more complete, more accurate, more nuanced. But there's
• 2:24:41
  a pattern emerging. The most powerful objects share characteristics. They
• 2:24:46
  involve extreme gravity, compact masses, high accretion rates, efficient energy conversion.
• 2:24:55
  They operate at the limits of physical law, maximum efficiency,
• 2:25:00
  optimal conditions. They're not common, rare events, special circumstances, but
• 2:25:06
  when they occur, they dominate. They outshine entire galaxies. They
• 2:25:12
  release more energy than billions of stars combined. They reshape
• 2:25:16
  their environments, create structures visible across cosmic distances. They're the
• 2:25:23
  universe showing what's possible when conditions are just right. Consider
• 2:25:28
  the physics involved. Einstein's equations allow for black holes, supermassive ones,
• 2:25:34
  stellar mass ones, intermediate mass ones. The math doesn't forbid them,
• 2:25:41
  it predicts them. General relativity describes spacetime curvature, how mass
• 2:25:47
  warps geometry, how extreme curvature creates event horizons, points of
• 2:25:53
  no return, the Schwarzchild radius, the boundary where escape velocity
• 2:25:58
  equals light speed inside nothing escapes outside everything's possible. The
• 2:26:05
  accretion disc forms outside matter, spirals inward friction heats it,
• 2:26:12
  Magnetic fields thread through it, instabilities develop, jets launch. The
• 2:26:18
  system self organizes into a power generator, converting gravitational potential
• 2:26:24
  energy into radiation into kinetic energy of outflows. The efficiency
• 2:26:29
  can reach thirty two percent, nearly a third of infalling
• 2:26:33
  mass becomes energy. Compare that to nuclear fusion. The Sun
• 2:26:38
  converts zero point seven percent less than one percent. Black
• 2:26:43
  Hole accretion is forty times more efficient. That's why quasers
• 2:26:48
  outshine galaxies, why active galactic nuclei dominate their hosts. The
• 2:26:55
  conversion mechanism is simply better, more effective, more powerful, and
• 2:27:01
  its scales Small black holes stellar mass can produce microquasars,
• 2:27:07
  smaller versions of the same phenomenon, but with lower total luminosity.
• 2:27:12
  Larger black holes supermassive can produce quasars ultra luminous agn
• 2:27:19
  The power scales with mass, with accretion rate, with efficiency.
• 2:27:24
  The biggest, fastest feeding black holes produce the most power.
• 2:27:29
  It's a direct relationship. More mass, more fuel, more output.
• 2:27:34
  The universe has tested this across cosmic time, across all
• 2:27:39
  mass ranges. The pattern holds black hole accretion is the
• 2:27:44
  most powerful sustained energy source we know, But what about
• 2:27:47
  transient events. Gamma ray bursts win that category. Brief intense, concentrated,
• 2:27:55
  a hypernova collapse, a neutron star merger. The energy release
• 2:28:01
  is explosive, sudden, in seconds, the output exceeds what the
• 2:28:06
  Sun produces in ten billion years. The peak luminosity is unmatched.
• 2:28:13
  Nothing shines brighter For those few seconds. The GRB is
• 2:28:19
  the most luminous object in the universe, visible across cosmic distances,
• 2:28:24
  detectable from the edge of the observable universe. Then it fades.
• 2:28:29
  The after glow persists days, weeks, months, but the peak passes.
• 2:28:36
  The event ends, the source becomes dormant, a black hole remains,
• 2:28:41
  a neutron star, an expanding debris cloud. The power was temporary, spectacular,
• 2:28:47
  but brief. So when we ask about the most powerful object,
• 2:28:51
  we need to specify time scales, sustained power quasas peak luminosity,
• 2:28:58
  gamma ray bursts, total energy release, the affucus, eruption, magnetic
• 2:29:05
  field strength, magnetars. Each category has its champion, each type
• 2:29:11
  of power has its exemplar. The universe contains multiple forms
• 2:29:15
  of extremity, different ways to be powerful, different mechanisms, different
• 2:29:22
  time scales, different manifestations. They're all real, all measurable, all
• 2:29:28
  operating within the same physical laws, but optimizing for different parameters.
• 2:29:34
  And we're still discovering, still observing. The next generation of
• 2:29:39
  telescopes will reveal more. The extremely large telescope thirty meters
• 2:29:45
  in diameter, ground based adaptive optics to correct for atmospheric distortion.
• 2:29:52
  It'll see further, resolve finer details, detect fainter objects. The
• 2:29:58
  square kilometer array radio telescope network spanning continents unprecedented sensitivity.
• 2:30:05
  It'll detect transient radio events, vast radio bursts, pulsar timing,
• 2:30:11
  quaser variability. The laser interferometer space antenna lyser A space
• 2:30:18
  based gravitational wave detector. Three spacecraft flying in formation millions
• 2:30:24
  of kilometers apart. It'll detect super massive black hole mergers,
• 2:30:30
  events invisible to ligo, too low frequency, too massive. These
• 2:30:37
  future instruments will expand our view, show us objects we
• 2:30:42
  can't currently detect. Events we're missing. The most powerful object
• 2:30:47
  might not have been found yet. It might be out
• 2:30:50
  there waiting beyond our current detection threshold. But based on
• 2:30:55
  what we know now the answer is clear for sustained
• 2:30:59
  luminosity quasers Reign Supreme Jay zero five two nine Dash
• 2:31:05
  four three five one currently holds the record fastest growing
• 2:31:10
  black hole, most luminous persistent source over five hundred trillion
• 2:31:15
  solar luminosities from a region smaller than our solar system.
• 2:31:21
  It's the most powerful object we've observed, the current champion
• 2:31:27
  until something brighter is discovered, until a more luminous quasar
• 2:31:31
  is found. The title is provisional, temporary, because the universe
• 2:31:38
  is vast, our surveys are incomplete, and somewhere in the
• 2:31:43
  cosmic dark, an even more powerful object might be shining, feeding, growing,
• 2:31:50
  converting mass to energy at rates we've never measured. We
• 2:31:54
  just haven't found it yet. But we're looking, and we'll
• 2:31:59
  keep looking, because that's what we do. We search for extremes.
• 2:32:04
  We measure the universe. We find the boundaries of what's possible,
• 2:32:09
  and when we discover the next record holder, we'll know
• 2:32:13
  where one step closer to understanding the full range of
• 2:32:17
  cosmic power, the complete spectrum of what reality allows, from
• 2:32:23
  the smallest particles to the largest structures, from quantum fluctuations
• 2:32:29
  to supermassive black holes, from the gentlest whisper to the
• 2:32:34
  loudest raw. The universe contains it all, and the most
• 2:32:39
  powerful object is simply the one that's found. The maximum,
• 2:32:43
  the peak, the upper limit, the answer to how powerful
• 2:32:48
  can anything possibly be? And now you know what that is.
• 2:32:52
  The universe operates at scales that make our most extreme
• 2:32:56
  achievements look quaint. Every nuclear weapon ever detonated combined wouldn't
• 2:33:02
  equal one second of a Magnetu's starquake. Every power plant
• 2:33:07
  on Earth running for a century wouldn't match the output
• 2:33:10
  of equasar for a microsecond. We've built machines that can
• 2:33:14
  split atoms, but the cosmos splits spacetime itself. And here's
• 2:33:20
  what's remarkable about that. We understand it, not just in
• 2:33:24
  vague terms. We can calculate the energies, we can measure
• 2:33:29
  the distances, we can predict the behavior. The equations describing
• 2:33:35
  a quasar's accretion disc are the same ones describing water
• 2:33:40
  swirling down a drain, just applied to regimes where gravity
• 2:33:45
  is strong enough to warp space, where velocities approach light speed,
• 2:33:51
  where temperatures reach millions of degrees. The physics doesn't change
• 2:33:57
  its scales. Maxwell's equations describe both the magnetic field and
• 2:34:02
  your refrigerator magnet and the quadrillion gorse field of a magnetar.
• 2:34:08
  Einstein's field equations govern both GPS satellites and black hole
• 2:34:14
  event horizons. The Nava Stokes equations apply to both coffee
• 2:34:19
  stirring in your cup and plasma flowing in an accretion
• 2:34:22
  disc same math, different parameters. That's the power of physical law,
• 2:34:29
  its universal, consistent, scalable. But understanding something doesn't diminish its magnificence.
• 2:34:39
  Knowing how a magnetar generates its field doesn't reduce the
• 2:34:43
  fact that it could kill you from a thousand kilometers
• 2:34:46
  away by destroying your atomic structure. Calculating Aquasa's luminosity doesn't
• 2:34:54
  change that it outshines hundreds of billions of stars. Measuring
• 2:34:59
  a gamma burst doesn't make it less impressive that it
• 2:35:03
  releases ten billion years of solar output in seconds. The
• 2:35:08
  numbers stand alone. They need no embellishment. Five hundred trillion
• 2:35:14
  solar luminosities, quadrillion gorse magnetic fields, energy outputs that dwarf
• 2:35:21
  the combined starlight of the observable universe. These aren't metaphors,
• 2:35:27
  their measurements actual values determined from actual observations. The universe
• 2:35:34
  genuinely produces phenomena at these scales, and we're part of it,
• 2:35:39
  not separate observers, but participants. The carbon in your DNA
• 2:35:44
  was forged in stellar corese The oxygen you breathe came
• 2:35:49
  from supernova explosions. The calcium in your bones was scattered
• 2:35:55
  by dying stars. You're constructed from the products of cosmic
• 2:35:59
  vs violence, made of star dust, literally, not poetically. Literally,
• 2:36:06
  that means when you observe a quasar, you're using atoms
• 2:36:10
  that once participated in similar processes. When you measure a
• 2:36:15
  gamma ray burst, you're employing elements created in comparable explosions.
• 2:36:21
  The subject and the observer are made of the same stuff,
• 2:36:25
  governed by the same laws, part of the same cosmic story,
• 2:36:31
  which makes the question of the most powerful object more
• 2:36:35
  than academic curiosity. It's about understanding the processes that created you,
• 2:36:42
  that shaped the matter comprising your body, that built the
• 2:36:46
  planet you stand on. The forces were describing aren't distant abstractions.
• 2:36:53
  They're the mechanisms that constructed reality itself. So what's the answer.
• 2:36:58
  What's the most powerful object in the universe depends on
• 2:37:02
  your metric Sustained electromagnetic luminosity points to j zero five
• 2:37:09
  two nine DASH four three five one, a quasar consuming
• 2:37:13
  more than a solar mass per day, radiating at five
• 2:37:17
  hundred trillion solar luminosities visible across twelve billion light years
• 2:37:22
  of expanding space. That's the current record holder for persistent brightness. Peak.
• 2:37:28
  Electromagnetic output points to gamma ray bursts g r B
• 2:37:34
  two two one zero zero nine, a released energy approaching
• 2:37:38
  the Sun's total rest mass in minutes, briefly outshone everything
• 2:37:44
  else in the universe at gamma ray wavelengths. That's the
• 2:37:47
  champion for explosive events. Magnetic field strength points to magnetars
• 2:37:53
  fields exceeding ten to the fifteenth gass a quadrillion times
• 2:37:59
  Earth's field, strong enough to warp atoms to alter vacuum
• 2:38:03
  properties to make space time itself behave differently. Gravitational wave
• 2:38:09
  luminosity points to merging supermassive black holes, two hundred million
• 2:38:14
  solar mass objects spiraling together in the final second. They
• 2:38:19
  emit more power in gravitational waves than all observable stars
• 2:38:24
  produce in light combined. That's the peak for space time distortion.
• 2:38:31
  Total energy release points to the ophucus eruption five point
• 2:38:36
  seven million times more energetic than the most powerful gamma
• 2:38:40
  ray burst, released over a hundred million years, creating structures
• 2:38:46
  visible across cosmological distances. That's the marathon champion. Each category
• 2:38:52
  has its winner, each form of power has its peak.
• 2:38:57
  The universe doesn't provide a single answer because power comes
• 2:39:00
  in multiple forms, different mechanisms, different time scales, different manifestations.
• 2:39:08
  They're all real, all extreme, all operating at the boundaries
• 2:39:12
  of physical law. But if forced to choose one answer
• 2:39:16
  for sustained power output measurable by human instruments, the title
• 2:39:20
  goes to J zero five two nine dash four three
• 2:39:26
  five one. The fastest growing black hole known, the most
• 2:39:31
  luminous persistent object detected. It represents the maximum steady state
• 2:39:36
  power we've observed, a super massive black hole feeding at
• 2:39:42
  near maximum efficiency, converting mass to energy at rates approaching
• 2:39:47
  theoretical limits, sustaining that output for millions of years, shaping
• 2:39:54
  its entire galactic environment. That's the most powerful object in
• 2:39:59
  the universe. Until we find something brighter, something more energetic,
• 2:40:05
  something that pushes even further against the limits of what
• 2:40:09
  physics allows. The surveys continue, the telescopes improve, the detection
• 2:40:15
  methods advance, and somewhere in the cosmic dark, an even
• 2:40:20
  more extreme object might be waiting, just beyond our current capabilities,
• 2:40:27
  ready to redefine what we mean by powerful. Because that's
• 2:40:31
  how science works. We find the current maximum, we study it,
• 2:40:36
  we understand it. Then we push further, look deeper, search harder,
• 2:40:43
  and eventually we find something more extreme. The process never ends.
• 2:40:49
  There's always another limit to test, another boundary to probe,
• 2:40:53
  another question to ask. The universe keeps providing answers, we
• 2:40:59
  keep asking questions, and in that dialogue between observation and theory,
• 2:41:05
  between measurement and prediction, we gradually map the full range
• 2:41:09
  of cosmic phenomena, from the gentlest whisper to the loudest roar,
• 2:41:16
  from quantum fluctuations to supermassive black holes, from the birth
• 2:41:21
  of atoms to the death of stars. It's all connected,
• 2:41:26
  all part of the same magnificent story. And the most
• 2:41:30
  powerful objects are simply the ones that found the maximum solution,
• 2:41:35
  the peak of what's possible, the upper limit of reality itself.