WEBVTT

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<v Speaker 1>Welcome to Bedtime Astronomy. Explore the wonders of the cosmos

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<v Speaker 1>with our soothing Bedtime Astronomie podcast. Each episode offers a

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<v Speaker 1>gentle journey through the stars, planets, and beyond, perfect for

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<v Speaker 1>unwinding after a long day. Let's travel through the mysteries

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<v Speaker 1>of the universe as you drift off into a peaceful

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<v Speaker 1>slumber under the night sky.

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<v Speaker 2>So I was actually walking through the Museum of Modern

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<v Speaker 2>Art a few months ago.

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<v Speaker 3>Oh nice, Yeah, trying to get.

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<v Speaker 2>Some culture, you know it is, And I found myself

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<v Speaker 2>just kind of standing in front of that small, almost

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<v Speaker 2>unassuming canvas by Salvat or.

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<v Speaker 3>Dolly the persistence of memory.

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<v Speaker 2>Exactly, the melting clocks, right, you know, the pocket watches

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<v Speaker 2>draped over dead tree branches and sliding off tables looking like,

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<v Speaker 2>I know, slices of cheese left out in the sun.

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<v Speaker 3>It is a very striking visual.

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<v Speaker 2>It really is. And usually when you look at that painting,

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<v Speaker 2>you think about the psychology of time. You think about

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<v Speaker 2>how an hour in a dentist's chair feels.

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<v Speaker 3>Like a week, Oh yeah, absolutely, and.

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<v Speaker 2>An hour with a good friend feels like a minute.

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<v Speaker 2>We did to think of memory and time as these

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<v Speaker 2>purely internal fluid.

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<v Speaker 3>Experiences, completely subjective, right.

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<v Speaker 2>Completely subjective. But standing there looking at those warped watches,

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<v Speaker 2>I started wondering, well, I started wondering if Dolly was

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<v Speaker 2>accidentally stumbling onto a literal truth about physics.

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<v Speaker 3>That is a fascinating leap, because we tend to think

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<v Speaker 3>of the physical universe, you know, the hard vacuum of

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<v Speaker 3>space as this rigid container.

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<v Speaker 2>A clock is a clock, a meter is a meter.

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<v Speaker 3>The stage where things happen exactly the stage.

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<v Speaker 2>But what if the contenter itself? What if the stage

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<v Speaker 2>actually melts? What if the universe has a memory and

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<v Speaker 2>that memory looks like a permanent physical distortion.

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<v Speaker 3>That is honestly the perfect mental anchor for what we

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<v Speaker 3>are unpacking today.

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<v Speaker 2>I thought it fit pretty well.

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<v Speaker 3>It does because in the world of general relativity, specifically

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<v Speaker 3>in the study of gravitational waves, there is a phenomenon

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<v Speaker 3>literally called memory capital M memory capital M, and it

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<v Speaker 3>suggests exactly what you just said. It suggests the universe

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<v Speaker 3>isn't just a static stage that events happen on. It

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<v Speaker 3>suggests the stage itself is recording the play.

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<v Speaker 2>And just so you listen, are clear, we aren't talking

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<v Speaker 2>about metaphor here, No, not at all. We aren't talking

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<v Speaker 2>about history in the sense of writing it down in

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<v Speaker 2>a physics textbook. We are talking about the actual fabric

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<v Speaker 2>of space time getting bent by a catastrophic event and then,

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<v Speaker 2>and this is the crazy part, never bending back.

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<v Speaker 3>That is the core concept. It is a permanent scar

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<v Speaker 3>on the geometry of reality.

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<v Speaker 2>A permanent scar. So for this deep dive, we are

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<v Speaker 2>looking at a brand new study. This is published in

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<v Speaker 2>Physical Review Letters in February twenty twenty.

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<v Speaker 3>Six rash off the presses, right.

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<v Speaker 2>It's titled the Persistence of Gravitational Wave Memory, and it's

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<v Speaker 2>led by Antonio Soccaros and his team.

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<v Speaker 3>Who are out of the University of Illinois at Urbana

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<v Speaker 3>Champagne and the Academy of Athens I believe, Yeah.

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<v Speaker 2>Along with with collaborators for the University of Valencia and

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<v Speaker 2>Montclair State. And they've basically been simulating what happens when

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<v Speaker 2>two of the most violent objects in the cosmos slam

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<v Speaker 2>into each.

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<v Speaker 3>Other binary neutron stars.

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<v Speaker 2>Right. And our mission today for this deep dive is

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<v Speaker 2>to really understand how the universe records its own history.

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<v Speaker 3>It is quite the mission.

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<v Speaker 2>It is we need to figure out why neutron stars

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<v Speaker 2>are so much more complicated than black holes, what role

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<v Speaker 2>ghost particles like Neutrino's playing all this, and ultimately why

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<v Speaker 2>this new study is considered such a massive stress test

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<v Speaker 2>for Einstein's theory.

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<v Speaker 3>It is the ultimate stress test, but it takes something

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<v Speaker 3>we thought we understood, gravitational waves, and adds a layer

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<v Speaker 3>of messiness that is frankly terrifying to simulate the mess.

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<v Speaker 2>We love the mess, But before we get to the

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<v Speaker 2>MESSI stress test, let's set the baseline good idea, because

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<v Speaker 2>we need to understand the difference between a ripple and

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<v Speaker 2>a scar. Most people listening have probably heard of gravitational

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<v Speaker 2>waves by now. Ligo detected them back in twenty fifteen.

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<v Speaker 3>Nobel prizes were handed.

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<v Speaker 2>Out exactly we know that and big things crash space ripples.

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<v Speaker 2>But to understand the new stuff, we need to know

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<v Speaker 2>what exactly we are crashing together in this specific study.

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<v Speaker 3>Right, so, we are looking at binary neutrons stars, two

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<v Speaker 3>neutron stars orbiting each other.

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<v Speaker 2>Give me the physical reality check here. I know they

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<v Speaker 2>are dense, but help me visualize what we're actually dealing with.

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<v Speaker 3>Sure, so imagine a star that started out much much

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<v Speaker 3>larger than our own Sun. It burns through all its

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<v Speaker 3>nuclear fuel over millions of years, and then the core collapses.

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<v Speaker 3>It goes supernova, the big boom, the biggest. The outer

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<v Speaker 3>layers blow off into space, but the core itself gets

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<v Speaker 3>crushed inwards by its own gravity. It is squeezing so

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<v Speaker 3>hard that the electrons and protons inside the atoms are

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<v Speaker 3>literally forced together to become neutrons.

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<v Speaker 2>So it's basically just a city sized atomic nucleus.

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<v Speaker 3>That's the classic analogy, and it holds up perfectly. You

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<v Speaker 3>have a perfect sphere, maybe twelve to fifteen miles across,

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<v Speaker 3>the size of Manhattan or London. Yeah, but it contains

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<v Speaker 3>up to two times the mass of our entire Sun.

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<v Speaker 2>That density is just it's hard to even wrap your

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<v Speaker 2>head around.

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<v Speaker 3>It is. Try this. If you took a teaspoon of

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<v Speaker 3>neutron star material, literally just a sugar cubesworth, it would

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<v Speaker 3>weigh about a billion tons.

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<v Speaker 2>A billion tons, Yeah, in a teaspoon.

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<v Speaker 3>That's roughly the weight of Mount Everest compressed into a spoon.

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<v Speaker 2>Okay, wow, So we are taking two of these Everest

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<v Speaker 2>spoon stars, spinning them around each other at a fraction

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<v Speaker 2>of the speed of light and just smashing them.

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<v Speaker 3>Together exactly, And as they spiral in towards each other,

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<v Speaker 3>they churn up the fabric of space time. They create

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<v Speaker 3>gravitational waves.

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<v Speaker 2>Now, the standard explanation, you know, the one I always

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<v Speaker 2>see in headlines, is the ripple in the pond analogy, right,

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<v Speaker 2>the classes You throw a rock into the water and

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<v Speaker 2>ripples move outwards. If I'm a rubber duck floating on

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<v Speaker 2>that pond, I just bob up and down as the

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<v Speaker 2>ripple goes by.

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<v Speaker 3>Right, And in this analogy, the rubber duck represents a

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<v Speaker 3>detector here on Earth, like Lego or maybe two astronauts

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<v Speaker 3>floating in space. Okay, As the gravitude wave passes through them,

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<v Speaker 3>the actual space between them stretches and squeezes. They get

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<v Speaker 3>closer than further, than closer than further, Bobby, exactly. That

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<v Speaker 3>is the oscillatory part of the wave, the back and forth.

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<v Speaker 2>And this is the key thing I want to focus on.

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<v Speaker 2>Once the wave passes, the bond goes flat again, the

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<v Speaker 2>rubbert duck ends up exactly where it started. The astronauts

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<v Speaker 2>return to their original distance.

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<v Speaker 3>That is what happens with a Spandard wave. Yes, it's temporary.

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<v Speaker 3>The universe is assumed to be elastic, it snaps back.

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<v Speaker 2>But the memory effect that this paper's about, yeah, says well,

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<v Speaker 2>it says that's wrong.

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<v Speaker 3>It says it's mostly right, but not entirely right. General

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<v Speaker 3>relativity actually predicts that, in addition to that back and

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<v Speaker 3>forth oscillation, there is a DC.

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<v Speaker 2>Component DC like direct current.

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<v Speaker 3>Yes, a direct current, a permanent offset.

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<v Speaker 2>So to go back to the astronauts in space.

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<v Speaker 3>The wave passes, they bob back and forth. But when

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<v Speaker 3>the wave is completely gone and space is quiet again,

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<v Speaker 3>they look at each other and realize they are now

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<v Speaker 3>slightly further apart or slightly closer together than they were

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<v Speaker 3>before the.

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<v Speaker 2>Wave hit, and they stay that way forever.

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<v Speaker 3>They do not snap back. The ruler itself has been

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<v Speaker 3>lengthened or shortened. Space time has been permanently displaced.

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<v Speaker 2>That is haunting. I mean, it implies that every single

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<v Speaker 2>time two black holes or neutron stars merge anywhere in

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<v Speaker 2>the universe, the geometry of the entire cosmos gets shifted

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<v Speaker 2>a tiny bit.

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<v Speaker 3>It does. It's a very very small shift, usually undetected

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<v Speaker 3>by our current instruments because it's so subtle. But mathematically

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<v Speaker 3>it has to be there the universe literally remembers the

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<v Speaker 3>event by changing its shape.

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<v Speaker 2>Okay, so that's the what. It's a permanent scar on reality.

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<v Speaker 2>But I really want to get into the why, because

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<v Speaker 2>looking at the history of this theory and the sources,

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<v Speaker 2>it seems like physicists have been arguing about this for

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<v Speaker 2>like fifty years.

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<v Speaker 3>Oh easily. It's definitely not a new idea. Even if

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<v Speaker 3>these specific supercomputer simulations are new. The foundation goes all

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<v Speaker 3>the way back to the nineteen seventies.

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<v Speaker 2>Nineteen seventy four with Zoldovich and.

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<v Speaker 3>Polmer f yes Yakov Zeldovitch and Alexander palm Reft, two

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<v Speaker 3>brilliant Soviet physicists. They were working with what we call

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<v Speaker 3>linearized gravity.

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<v Speaker 2>Linearized gravity, which is basically the light version of Einstein's equation.

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<v Speaker 3>Exactly the light version, the simpler approximation, and even in

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<v Speaker 3>that leet version, they realized that if you have a

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<v Speaker 3>system of stars that permanently changes its arrangement, say a

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<v Speaker 3>cluster of superdense stars suddenly flying apart, the gravitational field

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<v Speaker 3>at a great distance creates this prominent shift.

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<v Speaker 2>It was just a theoretical prediction at that.

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<v Speaker 3>Point, purely theoretical The logic was simple, though. If masses

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<v Speaker 3>move away to infinity, the metric of space time has to.

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<v Speaker 2>Change, so that's what we call the linear memory. The

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<v Speaker 2>stars moved, so the gravity changed basic cause and effect.

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<v Speaker 3>Right, But then came the nineties and things got profoundly weird.

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<v Speaker 2>Entered Demetrio's Christa d'lieu.

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<v Speaker 3>Yes. In nineteen ninety one, he published a paper that

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<v Speaker 3>is still considered a massive landmark in the field. He

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<v Speaker 3>didn't use the light version. He looked at the full,

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<v Speaker 3>unadulterated nonlinear Einstein equations.

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<v Speaker 2>I actually want to pause on that word. Non linear.

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<v Speaker 2>We hear it all the time, right, non linear dynamic

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<v Speaker 2>is non linear storytelling? In this context? Does it just

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<v Speaker 2>mean complicated?

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<v Speaker 3>It means that the output of a system literally becomes

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<v Speaker 3>an input for the system.

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<v Speaker 2>Okay, give me an example.

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<v Speaker 3>In a linear system, you have a choir singing. That's

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<v Speaker 3>the source, and the sound waves are the output. The

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<v Speaker 3>sound waves travel through the air to your ear. They

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<v Speaker 3>don't really interact with each other.

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<v Speaker 1>Right.

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<v Speaker 2>If the choir sing's louder, the sound is just louder.

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<v Speaker 2>It's a straight line from cause to effect exactly.

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<v Speaker 3>But in a nonlinear system, imagine the choir sings so

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<v Speaker 3>incredibly loud that the sound waves actually compress the air

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<v Speaker 3>enough to heat it up. That heat changes the density

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<v Speaker 3>of the air in the room, which then changes how

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<v Speaker 3>the sound travels, which might create entirely new sound frequencies.

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<v Speaker 3>The sound itself is changing the medium it travels through.

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<v Speaker 2>The output messages of the input. So apply that to gravity.

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<v Speaker 3>Well. Einstein's great insight was that mass equals energy E

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<v Speaker 3>equals mc squared. You have mass, you have gravity. But

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<v Speaker 3>if you have energy, you also have gravity.

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<v Speaker 2>And gravitational wave they carry energy exactly.

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<v Speaker 3>We know they carry energy because we can detect them.

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<v Speaker 3>They physically move the heavy mirrors in the Lego detectors.

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<v Speaker 3>That takes actual work. It takes energy. So Chris Dedooley realized,

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<v Speaker 3>if gravitational waves carry energy, then gravitational waves must have

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<v Speaker 3>their own gravitational feel Waitt.

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<v Speaker 2>The gravity has gravity.

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<v Speaker 3>The gravity has gravity.

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<v Speaker 2>That sounds like a recursive loop that would just immediately

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<v Speaker 2>crash a computer.

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<v Speaker 3>It makes the math incredibly difficult, which is exactly why

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<v Speaker 3>it took from nineteen seventy four until nineteen ninety one

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<v Speaker 3>to mathematically prove it. Christ to Doos showed that as

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<v Speaker 3>these waves ripple out from a collision, the massive energy

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<v Speaker 3>in the waves themselves creates a secondary gravitational distortion.

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<v Speaker 2>So it's not just the physical stars smashing together that

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<v Speaker 2>creates the memory scar it's the waves themselves piling up

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<v Speaker 2>as they travel.

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<v Speaker 3>Yes, this is called the nonlinear memory, where the Christad memory,

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<v Speaker 3>the waves effectively gravitate, They pull on space time as

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<v Speaker 3>they travel through it, and this effect accumulates. It builds

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<v Speaker 3>up over the entire duration of the wave signal.

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<v Speaker 2>So we have the linear memory, which is just the

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<v Speaker 2>stars moved, and the nonlinear memory, which is the energy

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<v Speaker 2>of the scream scarred the air.

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<v Speaker 3>That is a fantastic way to put it, the energy

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<v Speaker 3>of the scream scarred the air. And for a long time,

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<v Speaker 3>that combined picture was all we had, and we modeled

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<v Speaker 3>this mostly using.

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<v Speaker 2>Black holes because black holes are clean.

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<v Speaker 3>They are the simplest macroscopic objects in the universe. A

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<v Speaker 3>black hole has mass, it has spin, and it can

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<v Speaker 3>have an electric charge. That's it. No surface, no atmosphere,

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<v Speaker 3>no chemistry, just pure curved space time. So when you

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<v Speaker 3>program a computer to simulate two black holes merging, you

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<v Speaker 3>don't have to worry about fluid dynamics or magnetic fields

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<v Speaker 3>or particle physics. It's pure gravity.

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<v Speaker 2>But the universe isn't always clean, and that brings us

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<v Speaker 2>to the actual meat of the new study by Socaros

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<v Speaker 2>in his team. They didn't want the clean version. They

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<v Speaker 2>wanted the full messy reality of neutron stars.

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<v Speaker 3>And neutron stars are distinct because they are actual physical

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<v Speaker 3>objects made of ultra dense matter. They bring extra ingredients

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<v Speaker 3>to the party. They have magnetic fields, they emit light,

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<v Speaker 3>and crucially they emit neutrinos.

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<v Speaker 2>And so Kros is essentially asked, do these extra ingredients

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<v Speaker 2>actually contribute to the permanent space time scar? Yes, which

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<v Speaker 2>is a really fair question. Yeah, because if energy equals gravity,

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<v Speaker 2>and neutrinos carry energy and magnetic fields hold energy, shouldn't

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<v Speaker 2>they leave a mark too?

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<v Speaker 3>Exactly? And to be fair, previous researchers had laid the

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<v Speaker 3>groundwork for this, people like Lydia Bieri, Poning, Chen Shingtong Yao,

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<v Speaker 3>and Dave Garfinkel. They had done the pen and paper

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<v Speaker 3>math to prove that theoretically electromagnetic fields and neutrinos should

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<v Speaker 3>contribute to the memory.

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<v Speaker 2>I saw in the sources. This is sometimes called null memory.

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<v Speaker 3>Why null Oh? It relates to radiation traveling along what

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<v Speaker 3>physicists call null infinity, which is basically the mathematical boundary

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<v Speaker 3>or path that light, rays and massless particles take to

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<v Speaker 3>get infinitely far away from a source.

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<v Speaker 2>Nold infinity has to say, physics has the best names.

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<v Speaker 2>It sounds like an indie rock band.

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<v Speaker 3>It really does. But the point is, while the theory

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<v Speaker 3>for all memory was there, no one had successfully run

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<v Speaker 3>a full scale numerical relativity simulation of a binary neutron

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<v Speaker 3>star merger that actually quantified this.

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<v Speaker 2>No one, if we put numbers to it, right.

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<v Speaker 3>No oneted tract the neutrinos and the complex magnetic fields

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<v Speaker 3>and said, okay, here's exactly how much of the memory

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<v Speaker 3>they create until now.

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<v Speaker 2>So let's get into the simulation. They built a digital universe,

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<v Speaker 2>They put two massive neutron stars in it. They gave

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<v Speaker 2>them realistic magnetic fields and neutrino emissions. What did they find?

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<v Speaker 3>They found that the mess matters a lot.

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<v Speaker 2>Put a number on it for me.

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<v Speaker 3>The simulations suggest that the contributions from the extra ingredients,

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<v Speaker 3>the magnetic fields, the neutrinos, and the buryonic ejecta, which

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<v Speaker 3>is the physical matter thrown out of the crash. Account

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<v Speaker 3>for anyone where from fifteen percent to fifty percent of

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<v Speaker 3>the total gravitational wave memory.

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<v Speaker 2>Fifty percent up to half of the scar on the

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<v Speaker 2>universe is caused by the extras.

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<v Speaker 3>Yes, if you were to simulate this event and just

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<v Speaker 3>treat the neutron stars like black holes light, completely ignoring

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<v Speaker 3>the neutrinos in the matter, you could be wrong by

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<v Speaker 3>a factor of two. You'd be missing half the story.

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<v Speaker 2>That completely changes the picture. It means you absolutely cannot

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<v Speaker 2>just look at the gravity of the masses. You have

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<v Speaker 2>to look at the particle physics.

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<v Speaker 3>It forces a total marriage between gravity and nuclear physics.

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<v Speaker 2>Take the neutrinos for example. I usually think of them

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<v Speaker 2>as these ghostly little things that don't interact with anything,

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<v Speaker 2>like there are millions passing through.

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<v Speaker 3>My thumb right now, trillions actually trillions.

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<v Speaker 2>And normally they are totally gravitationally insignificant, right.

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<v Speaker 3>But a neutron star merger is not a normal environment.

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<v Speaker 3>When these stars crash together, the temperature spikes to billions

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<v Speaker 3>of degrees. The nuclear matter is literally being crushed and

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<v Speaker 3>boiled at the same time.

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<v Speaker 2>What does that do.

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<v Speaker 3>It releases a flood of neutrinos that is frankly hard

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<v Speaker 3>to comprehend. The paper mentions a total energy release of

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<v Speaker 3>around ten to the fifty three ergs.

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<v Speaker 2>Yeah, I saw that, and I know ergs is a

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<v Speaker 2>unit of energy, but I have zero intuition for that

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<v Speaker 2>is ten to the fifty three a lot.

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<v Speaker 3>It's an astronomical number. For context, our Sun over its

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<v Speaker 3>entire ten billion year lifespan will emit something like ten

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<v Speaker 3>to the fifty one ergs of energy.

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<v Speaker 2>Wait, so this single crash releases one hundred times more

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<v Speaker 2>energy in just a few seconds just in neutrinos than

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<v Speaker 2>the Sun does in its entire ten billion year life.

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<v Speaker 3>Exactly. It is a sudden explosion of energy that briefly

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<v Speaker 3>outshines the entire galaxy in neutrino radiation. And because E

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<v Speaker 3>equals mc squared, that massive energy has a mass equivalence.

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<v Speaker 2>So as these trillions of neutrinos stream out of the

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<v Speaker 2>crash site in all directions, they're effectively carrying an immense

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<v Speaker 2>amount of mass away with them.

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<v Speaker 3>Right, imagine the crash site is losing weight incredibly rapidly.

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<v Speaker 3>That sudden chain in the mass distribution that lightning of

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<v Speaker 3>the central load causes a massive shift in the gravitational

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<v Speaker 3>field that is the neutrino memory.

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<v Speaker 2>It's like if you were standing on a trampoline holding

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<v Speaker 2>a heavy bowling ball. The trampoline is curved down around you.

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<v Speaker 2>If you suddenly throw the bowling ball away, the trampoline

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<v Speaker 2>snaps to a new shallower shape.

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<v Speaker 3>That's a very good analogy for the linear part of it.

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<v Speaker 3>The mass has moved, so the curve changes. But there's

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<v Speaker 3>also the nonlinear part we talked about. The neutrinos themselves

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<v Speaker 3>are dragging space time as they fly outward, and the

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<v Speaker 3>study showed this combined effect is a huge component of

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<v Speaker 3>the final memory signal.

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<v Speaker 2>And there's a specific visualization in the paper they mentioned

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<v Speaker 2>that really caught my eye. A blue rectangle. Can you

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<v Speaker 2>describe what we're looking at there?

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<v Speaker 3>Sure? So this is a graph showing the strain, basically,

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<v Speaker 3>the memory accumulation over time. On the horizontal axis you

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<v Speaker 3>have time in milliseconds. On the vertical axis, you have

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<v Speaker 3>the memory building up.

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<v Speaker 2>And what exactly does the blue rectangle highlight?

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<v Speaker 3>It highlights the time duration over which ninety percent of

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<v Speaker 3>the post merger memory is accumulated. For a black hole merger.

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<v Speaker 3>The memory happens in a literal snap. It's a step

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<v Speaker 3>function on a graph. Nothing nothing s and app full memory,

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<v Speaker 3>instant scarring. But for neutron stars, the blue rectangle shows

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<v Speaker 3>that the memory builds up gradually. It takes tens of milliseconds,

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<v Speaker 3>which sounds fast, but is an absolute eternity in this

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<v Speaker 3>specific physics context for the memory to reach its full height.

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<v Speaker 2>Why the delay? Why doesn't it just snap like a

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<v Speaker 2>black hole.

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<v Speaker 3>Because the neutrinos take time to leak out of the

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<v Speaker 3>ultra dense core. The ejected matter, these massive clouds of

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<v Speaker 3>gold and platinum dust, takes time to expand outward, and

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<v Speaker 3>the remnant itself, the hyper massive blob of matter left

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<v Speaker 3>over from the crash, wobbles and slashes around for a

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<v Speaker 3>while before finally settling down.

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<v Speaker 2>So it's a slow motion scar exactly.

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<v Speaker 3>And that slope how fast or slow the memory builds

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<v Speaker 3>up tells you immense amounts about the internal physics of

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<v Speaker 3>the explasion.

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<v Speaker 2>Now, speaking of the internal physics, we have to talk

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<v Speaker 2>about the magnetic fields because this is where my own

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<v Speaker 2>naive assumption totally failed me.

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<v Speaker 3>While I was reading what was your assumption.

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<v Speaker 2>Okay, so my logic was pretty straightforward. I know these

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<v Speaker 2>stars are giant magnets. Magnetars are some of the scariest

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<v Speaker 2>things in space, and I know energy equals gravity. Magnetic

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<v Speaker 2>fields contain energy.

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<v Speaker 3>Solid logic, so far right.

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<v Speaker 2>So if I take two stars with super strong magnetic

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<v Speaker 2>fields and smash them together, I'm adding more energy to

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<v Speaker 2>the whole system than if they were unmagnetized. More energy

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<v Speaker 2>should mean more gravity, which should mean a much bigger

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<v Speaker 2>memory scar.

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<v Speaker 3>That is entirely logical. It is what we call the

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<v Speaker 3>naive expectation. And I don't mean that as an insult

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<v Speaker 3>at all. It's exactly what many physicists expected too before

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<v Speaker 3>they ran the numbers.

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<v Speaker 2>But the simulation said no.

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<v Speaker 3>The simulation showed that in some cases, adding incredibly strong

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<v Speaker 3>magnetic fields actually reduced the final gravitational wave memory.

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<v Speaker 2>How was that possible? Where did all that magnetic energy go?

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<v Speaker 3>The energy is absolutely there, but it's not making gravitational waves.

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<v Speaker 3>You have to remember a key rule. Gravitational waves are

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<v Speaker 3>generated by asymmetry.

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00:19:01.119 --> 00:19:02.599
<v Speaker 2>Asymmetry, yes, they are.

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<v Speaker 3>Generated by what we call the quadrupole moment. Basically, you

399
00:19:06.039 --> 00:19:10.240
<v Speaker 3>need a lumpy, uneven wobbling distribution of mass to shake

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00:19:10.319 --> 00:19:10.960
<v Speaker 3>space time.

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00:19:11.200 --> 00:19:13.039
<v Speaker 2>A perfect sphere doesn't make waves.

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00:19:13.359 --> 00:19:16.920
<v Speaker 3>Correct. Even if the perfect sphere is spinning incredibly fast,

403
00:19:17.240 --> 00:19:21.400
<v Speaker 3>it is symmetric, no waves are produced. You need the wobble. Okay, now,

404
00:19:21.440 --> 00:19:24.359
<v Speaker 3>think about what a strong magnetic field does to a

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00:19:24.400 --> 00:19:27.559
<v Speaker 3>ball of highly conducting fluid, which is essentially what a

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00:19:27.559 --> 00:19:28.680
<v Speaker 3>hot neutron star is.

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00:19:28.839 --> 00:19:29.680
<v Speaker 2>It holds it together.

408
00:19:29.920 --> 00:19:34.000
<v Speaker 3>It creates magnetic viscosity. It creates tension. Imagine stirring a

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00:19:34.039 --> 00:19:38.119
<v Speaker 3>cup of water with a spoon. It splashes everywhere, it swirls.

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00:19:38.359 --> 00:19:42.440
<v Speaker 3>It's highly turbulent and chaotic. Right now, imagine stirring a

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00:19:42.480 --> 00:19:44.400
<v Speaker 3>cup of cold honey or molasses.

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00:19:44.480 --> 00:19:46.200
<v Speaker 2>It moves way slower. It's stiff.

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00:19:46.359 --> 00:19:50.599
<v Speaker 3>Exactly. The strong magnetic field acts like a stiffener. It

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00:19:50.720 --> 00:19:54.279
<v Speaker 3>links the fluid elements inside the star together when the

415
00:19:54.319 --> 00:19:57.799
<v Speaker 3>stars crash. If the magnetic field is strong enough and

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00:19:57.880 --> 00:20:01.759
<v Speaker 3>shaped a certain way, it actually suppresses the fluid turbulence.

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00:20:02.119 --> 00:20:06.400
<v Speaker 3>It prevents the massive sloshing and forces the resulting merged

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00:20:06.480 --> 00:20:09.799
<v Speaker 3>blob into a more symmetric, stable shape much faster.

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00:20:10.200 --> 00:20:12.559
<v Speaker 2>So the magnetic field acts like a straight jacket for

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00:20:12.599 --> 00:20:16.200
<v Speaker 2>the star. It stops the blob from slashing around as much.

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00:20:16.000 --> 00:20:19.279
<v Speaker 3>And less slashing means less asymmetry. Less asymmetry means less

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00:20:19.279 --> 00:20:23.000
<v Speaker 3>gravitational radiation. So even though you have physically more energy

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00:20:23.119 --> 00:20:25.960
<v Speaker 3>stored in the magnetic field itself, you have less dynamic

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00:20:26.039 --> 00:20:27.799
<v Speaker 3>shaking to create the memory signal.

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00:20:27.920 --> 00:20:31.400
<v Speaker 2>That is wildly counterintuitive. It's like saying that crashing a

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00:20:31.440 --> 00:20:34.559
<v Speaker 2>sports car at high speed might actually do less structural

427
00:20:34.640 --> 00:20:36.839
<v Speaker 2>damage to the environment if the car is made of

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00:20:36.839 --> 00:20:38.000
<v Speaker 2>a much stiffer material.

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00:20:38.279 --> 00:20:41.519
<v Speaker 3>In a way, yes, the internal dynamics matter more than

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00:20:41.559 --> 00:20:44.599
<v Speaker 3>the raw energy count alone, and the study found this

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00:20:44.680 --> 00:20:48.039
<v Speaker 3>memory dampening depends heavily on the topology of the field.

432
00:20:48.640 --> 00:20:51.640
<v Speaker 2>Copology that just means the shape of the magnetic field right.

433
00:20:51.599 --> 00:20:55.880
<v Speaker 3>Yes, is the magnetic field aligned perfectly with the star's spin?

434
00:20:56.640 --> 00:21:00.880
<v Speaker 3>Is it tilted perpendicular? Is it a toroidal field meaning

435
00:21:00.920 --> 00:21:04.519
<v Speaker 3>it's shaped like a doughnut entirely inside the star. The

436
00:21:04.559 --> 00:21:07.680
<v Speaker 3>study showed an intricate dependence on these shapes.

437
00:21:07.440 --> 00:21:10.000
<v Speaker 2>Meaning you can't just guess the outcome based on energy.

438
00:21:10.160 --> 00:21:12.640
<v Speaker 3>You absolutely cannot guess. You have to run the supercomputer

439
00:21:12.720 --> 00:21:14.519
<v Speaker 3>code for every specific scenario.

440
00:21:14.799 --> 00:21:18.880
<v Speaker 2>This brings us to the real face. So what of

441
00:21:18.920 --> 00:21:22.160
<v Speaker 2>the episode We've got these amazing simulations. We know that

442
00:21:22.240 --> 00:21:25.400
<v Speaker 2>neutrinos and magnets and gold dust all contribute up to

443
00:21:25.440 --> 00:21:27.759
<v Speaker 2>half of this scar in the universe. But we haven't

444
00:21:27.759 --> 00:21:30.119
<v Speaker 2>actually seen this yet, have we. Logo hasn't flashed a

445
00:21:30.160 --> 00:21:31.640
<v Speaker 2>red light saying memory detected.

446
00:21:31.839 --> 00:21:35.400
<v Speaker 3>Not yet. No, we have successfully detected the oscillatory waves,

447
00:21:35.519 --> 00:21:38.079
<v Speaker 3>the chirp of the merger as they spiral in. But

448
00:21:38.160 --> 00:21:40.799
<v Speaker 3>the memory is a very low frequency effect. It's a

449
00:21:40.839 --> 00:21:43.920
<v Speaker 3>permanent DC offset, and current detectors just can't see that.

450
00:21:44.240 --> 00:21:47.799
<v Speaker 3>Current ground based detectors like LIGO are not great at

451
00:21:47.799 --> 00:21:50.160
<v Speaker 3>seeing things that happen slowly or just stay put.

452
00:21:50.359 --> 00:21:52.880
<v Speaker 2>Why is that because of the Earth exactly.

453
00:21:53.400 --> 00:21:56.039
<v Speaker 3>Think about how LIGO actually works. It's a series of

454
00:21:56.079 --> 00:21:59.680
<v Speaker 3>heavy mirrors hanging on delicate glass threads. It's looking for

455
00:21:59.759 --> 00:22:03.359
<v Speaker 3>high frequency vibrations. If the mirror moves and then just

456
00:22:03.400 --> 00:22:06.519
<v Speaker 3>stays moved, it's incredibly hard for the computer to tell

457
00:22:06.599 --> 00:22:09.480
<v Speaker 3>if that was a permanent gravitational wave memory, or if

458
00:22:09.519 --> 00:22:12.160
<v Speaker 3>the tectonic plate under the building just shifted slightly, or

459
00:22:12.160 --> 00:22:14.559
<v Speaker 3>if a truck drove by, or even if the laser

460
00:22:14.640 --> 00:22:15.920
<v Speaker 3>slightly heated up the mirror.

461
00:22:16.079 --> 00:22:18.720
<v Speaker 2>The permanent shift just gets lost in the everyday noise

462
00:22:18.720 --> 00:22:19.279
<v Speaker 2>of the planet.

463
00:22:19.359 --> 00:22:22.559
<v Speaker 3>It just looks like instrument drift. But with next generation

464
00:22:22.680 --> 00:22:25.519
<v Speaker 3>detectors like the Einstein Telescope, which they are planning to

465
00:22:25.519 --> 00:22:28.920
<v Speaker 3>build deep underground in Europe, or LYSA, which will be

466
00:22:28.960 --> 00:22:32.119
<v Speaker 3>a triangle of satellites flying millions of miles apart in space,

467
00:22:32.720 --> 00:22:35.759
<v Speaker 3>we should finally be able to separate this subtle memory

468
00:22:35.799 --> 00:22:37.119
<v Speaker 3>signal from the noise.

469
00:22:37.440 --> 00:22:40.000
<v Speaker 2>And when we do find it, what does it actually

470
00:22:40.039 --> 00:22:44.039
<v Speaker 2>tell us? Why are so many physicists dedicating their careers

471
00:22:44.359 --> 00:22:45.759
<v Speaker 2>to hunting for this scar.

472
00:22:45.799 --> 00:22:48.480
<v Speaker 3>Because it is the ultimate forensic tool. If we can

473
00:22:48.559 --> 00:22:52.200
<v Speaker 3>cleanly read the memory signal, we can essentially reverse engineer

474
00:22:52.240 --> 00:22:52.799
<v Speaker 3>the dead star.

475
00:22:53.039 --> 00:22:54.960
<v Speaker 2>This connects back to a term I saw all over

476
00:22:55.000 --> 00:22:59.079
<v Speaker 2>the sources, equation of state. I really want to drill

477
00:22:59.119 --> 00:23:02.359
<v Speaker 2>down this. What exactly is an equation of state?

478
00:23:03.000 --> 00:23:06.119
<v Speaker 3>In physics? An equation of state is simply a mathematical

479
00:23:06.200 --> 00:23:09.440
<v Speaker 3>rule that connects density to pressure. For the air in

480
00:23:09.480 --> 00:23:12.119
<v Speaker 3>your car tire, it's simple physics. You can press it

481
00:23:12.119 --> 00:23:15.279
<v Speaker 3>the pressure goes up linearly. But for the exotic matter

482
00:23:15.319 --> 00:23:18.000
<v Speaker 3>inside a neutron star, we genuinely don't know the rule

483
00:23:18.319 --> 00:23:18.759
<v Speaker 3>because we.

484
00:23:18.720 --> 00:23:21.039
<v Speaker 2>Can't build a neutron star in a lab on Earth

485
00:23:21.079 --> 00:23:22.039
<v Speaker 2>to test it right.

486
00:23:22.240 --> 00:23:25.640
<v Speaker 3>We cannot squeeze normal matter to nuclear densities on Earth

487
00:23:25.680 --> 00:23:28.039
<v Speaker 3>without it just becoming a bomb. So we don't know

488
00:23:28.079 --> 00:23:30.480
<v Speaker 3>what happens at the very core. Is the core squishy,

489
00:23:30.599 --> 00:23:33.680
<v Speaker 3>is it extremely stiff, Is it made of regular free neutrons,

490
00:23:33.759 --> 00:23:36.559
<v Speaker 3>or does it melt down into a bizarre soup of

491
00:23:36.720 --> 00:23:38.599
<v Speaker 3>free quirks. We just don't know.

492
00:23:38.759 --> 00:23:42.440
<v Speaker 2>And whether it's stiff or squishy changes how it crashes drastically.

493
00:23:43.000 --> 00:23:47.480
<v Speaker 3>A stiff star strongly resists collapsing it bounces. A soft,

494
00:23:47.599 --> 00:23:52.279
<v Speaker 3>squishy star smushes together very easily. That physical difference changes

495
00:23:52.279 --> 00:23:54.880
<v Speaker 3>how the whole merger happens, which changes the shape of

496
00:23:54.920 --> 00:23:58.680
<v Speaker 3>the gravitational waves, which ultimately changes the slope and size

497
00:23:58.680 --> 00:23:59.880
<v Speaker 3>of the permanent memory scar.

498
00:24:00.279 --> 00:24:02.960
<v Speaker 2>So if we detect the memory scar with Lisa, we

499
00:24:02.960 --> 00:24:06.039
<v Speaker 2>could look at its precise shape and say, Aha, that

500
00:24:06.200 --> 00:24:10.359
<v Speaker 2>scar means the star was squishy. Therefore the core couldn't

501
00:24:10.359 --> 00:24:12.599
<v Speaker 2>have been pure quark matter precisely.

502
00:24:13.039 --> 00:24:16.799
<v Speaker 3>The space time memory inherently encodes the hidden nuclear physics

503
00:24:16.799 --> 00:24:18.960
<v Speaker 3>of the core. It's a way to look deep inside

504
00:24:18.960 --> 00:24:20.960
<v Speaker 3>an object that we can never ever visit.

505
00:24:20.960 --> 00:24:23.759
<v Speaker 2>And beyond the forensics of the star itself, it's also

506
00:24:23.839 --> 00:24:26.400
<v Speaker 2>a massive test for the fundamental theory of gravity.

507
00:24:26.759 --> 00:24:28.519
<v Speaker 3>It is the stress test we mentioned at the start.

508
00:24:28.880 --> 00:24:31.559
<v Speaker 3>General relativity is over one hundred years old now it

509
00:24:31.599 --> 00:24:33.680
<v Speaker 3>has famously passed every single test.

510
00:24:33.440 --> 00:24:35.160
<v Speaker 2>We've thrown at it, every single one.

511
00:24:35.279 --> 00:24:38.240
<v Speaker 3>But the memory effect relies heavily on that nonlinearity. We

512
00:24:38.319 --> 00:24:42.319
<v Speaker 3>discussed the wild idea that gravity creates its own gravity.

513
00:24:42.440 --> 00:24:44.359
<v Speaker 2>So if we build Lisa and we look for the

514
00:24:44.400 --> 00:24:46.920
<v Speaker 2>memory exactly where the simulations say it should be and

515
00:24:46.960 --> 00:24:48.240
<v Speaker 2>it's just not there.

516
00:24:48.039 --> 00:24:51.279
<v Speaker 3>Then Einstein was wrong, or at the very least his

517
00:24:51.400 --> 00:24:54.079
<v Speaker 3>theory breaks down at these extreme high energies.

518
00:24:54.519 --> 00:24:56.640
<v Speaker 2>That would be the biggest news in physics in a century.

519
00:24:56.720 --> 00:24:59.680
<v Speaker 3>It really would. Or more likely, maybe we find the

520
00:24:59.720 --> 00:25:03.880
<v Speaker 3>memory but it looks totally different than Sakarosa's simulations predict

521
00:25:04.240 --> 00:25:06.559
<v Speaker 3>That would tell us we don't understand Neutrino's nearly as

522
00:25:06.599 --> 00:25:08.880
<v Speaker 3>well as we thought, or that matter behaves in some

523
00:25:09.039 --> 00:25:12.200
<v Speaker 3>entirely new way when extreme magnetic fields are involved.

524
00:25:12.440 --> 00:25:16.119
<v Speaker 2>It's a win win for science. Either we definitively confirm

525
00:25:16.200 --> 00:25:19.039
<v Speaker 2>the wildest prediction of the theory, or we break the

526
00:25:19.039 --> 00:25:20.799
<v Speaker 2>theory and find new physics.

527
00:25:21.039 --> 00:25:23.759
<v Speaker 3>That's the beauty of experimental astrophysics.

528
00:25:23.839 --> 00:25:25.319
<v Speaker 2>I want to zoom out a bit as we wrap

529
00:25:25.400 --> 00:25:27.519
<v Speaker 2>up here. We've been talking heavily about the math and

530
00:25:27.559 --> 00:25:30.440
<v Speaker 2>neutrinos and fluid dynamics, but I keep coming back to

531
00:25:30.480 --> 00:25:33.000
<v Speaker 2>that Dolly painting in the museum. And there was a

532
00:25:33.039 --> 00:25:35.880
<v Speaker 2>specific quote from Sacroo's in the press release that really

533
00:25:35.880 --> 00:25:36.319
<v Speaker 2>struck me.

534
00:25:36.480 --> 00:25:37.960
<v Speaker 3>Ah, the one about the worldline.

535
00:25:38.039 --> 00:25:42.279
<v Speaker 2>Yeah, he said, similarly to our own persistent memory, which

536
00:25:42.319 --> 00:25:45.920
<v Speaker 2>is shaped by the worldline of our lives, binary compact

537
00:25:46.000 --> 00:25:50.200
<v Speaker 2>objects also develop a persistent memory, as described by Einstein's

538
00:25:50.240 --> 00:25:51.039
<v Speaker 2>theory of gravity.

539
00:25:51.319 --> 00:25:54.519
<v Speaker 3>It's a beautifully poetic connection for a physicist to make.

540
00:25:55.079 --> 00:25:58.640
<v Speaker 3>In relativity, a world line is just your path through

541
00:25:58.680 --> 00:26:01.359
<v Speaker 3>four dimensional space time from the moment of your birth

542
00:26:01.400 --> 00:26:04.160
<v Speaker 3>to your death. You trace a unique line.

543
00:26:04.720 --> 00:26:07.039
<v Speaker 2>And he's essentially saying that, just like our lives leave

544
00:26:07.039 --> 00:26:10.720
<v Speaker 2>physical memories in the neurons of our brains, the violent

545
00:26:10.799 --> 00:26:14.200
<v Speaker 2>lives of these stars leave actual physical memories in the

546
00:26:14.200 --> 00:26:15.759
<v Speaker 2>fabric of the universe itself.

547
00:26:15.960 --> 00:26:18.640
<v Speaker 3>It implies that the deep history of the cosmos isn't

548
00:26:18.680 --> 00:26:22.759
<v Speaker 3>just gone, it's physically recorded. The geometry of the universe

549
00:26:22.880 --> 00:26:26.000
<v Speaker 3>right now today is the cumulative some of all the

550
00:26:26.079 --> 00:26:29.480
<v Speaker 3>massive collisions and mergers that have ever happened since the

551
00:26:29.519 --> 00:26:30.480
<v Speaker 3>Big Bang.

552
00:26:30.279 --> 00:26:32.160
<v Speaker 2>Which leads to a sort of terrifying thought for me.

553
00:26:32.359 --> 00:26:34.720
<v Speaker 2>If these mergers have been happening for billions of years

554
00:26:34.759 --> 00:26:38.119
<v Speaker 2>across the whole universe, billions of black holes, billions of

555
00:26:38.119 --> 00:26:41.839
<v Speaker 2>neutron stars, and each single one stretches space a tiny

556
00:26:41.880 --> 00:26:44.319
<v Speaker 2>little bit and leaves a permanent scar.

557
00:26:44.720 --> 00:26:47.240
<v Speaker 3>You're wondering if the universe is getting wrinkly, I.

558
00:26:47.240 --> 00:26:50.240
<v Speaker 2>Am, is the universe smoother in the distant past and

559
00:26:50.279 --> 00:26:53.759
<v Speaker 2>more discorded now, or we essentially accumulating cosmic trauma in

560
00:26:53.799 --> 00:26:54.319
<v Speaker 2>a very.

561
00:26:54.240 --> 00:26:58.200
<v Speaker 3>Real mathematical sense, Yes, the texture of the gravitational field

562
00:26:58.240 --> 00:27:02.039
<v Speaker 3>is getting richer, more complex. It's constantly being worked over

563
00:27:02.119 --> 00:27:05.200
<v Speaker 3>by these extreme events. We are living in a universe

564
00:27:05.240 --> 00:27:09.799
<v Speaker 3>that is physically geometrically different than it was yesterday, precisely

565
00:27:09.880 --> 00:27:12.319
<v Speaker 3>because of the events that happened today.

566
00:27:12.400 --> 00:27:14.720
<v Speaker 2>We aren't just actors on a stage. We're on the

567
00:27:14.759 --> 00:27:18.200
<v Speaker 2>states that is constantly warping and stretching beneath our feet, and.

568
00:27:18.119 --> 00:27:20.440
<v Speaker 3>Thanks to studies like this one, we are just now

569
00:27:20.519 --> 00:27:22.039
<v Speaker 3>learning how to read those warps.

570
00:27:22.359 --> 00:27:25.559
<v Speaker 2>So what's next? For the team. They've proved the concept

571
00:27:26.039 --> 00:27:26.960
<v Speaker 2>with this simulation.

572
00:27:27.319 --> 00:27:30.599
<v Speaker 3>Sakaros calls this a first Foray. Now comes the real

573
00:27:30.680 --> 00:27:34.200
<v Speaker 3>computational grind. They need to run hundreds, maybe thousands of

574
00:27:34.240 --> 00:27:38.200
<v Speaker 3>these simulations, tweaking all the variables right, different masses, different

575
00:27:38.279 --> 00:27:41.960
<v Speaker 3>magnetic field shapes, different equations of state for the core.

576
00:27:42.200 --> 00:27:44.039
<v Speaker 2>That basically need to build a library.

577
00:27:44.000 --> 00:27:47.640
<v Speaker 3>Exactly, a comprehensive catalog, so when Lisa or the Einstein

578
00:27:47.640 --> 00:27:50.599
<v Speaker 3>Telescope finally turns on and catches a memory signal, the

579
00:27:50.640 --> 00:27:52.680
<v Speaker 3>scientist can look it up in the library and say, oh,

580
00:27:52.720 --> 00:27:56.200
<v Speaker 3>that matches simulation four hundred exactly. It was a one

581
00:27:56.240 --> 00:28:00.240
<v Speaker 3>point four solar mass binary with a stiff core and

582
00:28:00.319 --> 00:28:02.279
<v Speaker 3>ateroidal magnetic.

583
00:28:01.799 --> 00:28:04.519
<v Speaker 2>Field, decoding the universe's scars.

584
00:28:04.359 --> 00:28:07.440
<v Speaker 3>Multi messenger astronomy at its absolute finest.

585
00:28:07.559 --> 00:28:10.839
<v Speaker 2>Well, my brain is suitably stretched. For one day, we

586
00:28:10.880 --> 00:28:12.880
<v Speaker 2>went from melting clocks in New York to the density

587
00:28:12.880 --> 00:28:15.920
<v Speaker 2>Mount Everest and at scone to the mind bending idea

588
00:28:15.960 --> 00:28:17.359
<v Speaker 2>that gravity itself has weight.

589
00:28:17.599 --> 00:28:19.480
<v Speaker 3>Just another day in astrophysics to.

590
00:28:19.480 --> 00:28:21.480
<v Speaker 2>Recap for everyone listening out there, So you have this

591
00:28:21.599 --> 00:28:25.200
<v Speaker 2>locked in one space. Time isn't rigid, It has a memory.

592
00:28:25.559 --> 00:28:28.599
<v Speaker 2>Big crashes leave permanent physical scars on the geometry of

593
00:28:28.599 --> 00:28:33.599
<v Speaker 2>the universe. Two neutron star mergers are incredibly messy. You

594
00:28:33.680 --> 00:28:37.599
<v Speaker 2>absolutely cannot ignore the extra ingredients. Neutrinos and ejected matter

595
00:28:37.640 --> 00:28:39.480
<v Speaker 2>account for up to half of that memory signal.

596
00:28:39.519 --> 00:28:40.319
<v Speaker 3>It mass matters.

597
00:28:40.519 --> 00:28:43.359
<v Speaker 2>Three magnetism is weird. It can actually reduce the toll

598
00:28:43.480 --> 00:28:46.440
<v Speaker 2>memory signal by stiffening the star and making the resulting

599
00:28:46.519 --> 00:28:48.400
<v Speaker 2>crash smoother and more symmetrical.

600
00:28:48.519 --> 00:28:53.440
<v Speaker 3>The counterintuitive finding and four detecting this memory is how

601
00:28:53.440 --> 00:28:56.319
<v Speaker 3>we eventually crack open the neutron star to see what's

602
00:28:56.319 --> 00:28:59.839
<v Speaker 3>actually inside the core. A perfect summary, I want to leave.

603
00:28:59.759 --> 00:29:02.839
<v Speaker 2>You with one final provocative thought. Today we talked a

604
00:29:02.880 --> 00:29:07.079
<v Speaker 2>lot about the universe remembering about carrying the physical record

605
00:29:07.119 --> 00:29:10.240
<v Speaker 2>of its own violent past. We usually think of the

606
00:29:10.319 --> 00:29:16.119
<v Speaker 2>laws of physics as completely timeless, eternal. But if the

607
00:29:16.160 --> 00:29:20.519
<v Speaker 2>actual structure of space itself is continuously evolving, if it's

608
00:29:20.559 --> 00:29:25.440
<v Speaker 2>constantly accumulating these tiny permanent shifts, these memories, right, does

609
00:29:25.440 --> 00:29:27.880
<v Speaker 2>that mean the universe we live in today is fundamentally

610
00:29:27.960 --> 00:29:31.079
<v Speaker 2>structurally different from the universe of the Big Bang, not

611
00:29:31.160 --> 00:29:34.240
<v Speaker 2>just because it's older or larger, but because it's scarred.

612
00:29:35.039 --> 00:29:37.519
<v Speaker 2>Is the gravity holding you to the ground today exactly

613
00:29:37.559 --> 00:29:39.599
<v Speaker 2>the same as gravity yesterday. Or are we all just

614
00:29:39.640 --> 00:29:43.920
<v Speaker 2>floating in the microscopic wreckage of a billion cosmic car crashes,

615
00:29:44.160 --> 00:29:46.000
<v Speaker 2>finally trying to make sense of the damage.

616
00:29:46.079 --> 00:29:47.880
<v Speaker 3>That is a very heavy thought to end on.

617
00:29:48.039 --> 00:29:50.599
<v Speaker 2>That's exactly why we call it the deep dive. Thanks

618
00:29:50.640 --> 00:29:53.039
<v Speaker 2>for listening, everyone, keep looking up. See next time.

619
00:30:03.079 --> 00:30:37.000
<v Speaker 3>Us SA
