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Speaker 1: Hey, Daniel, I have a question about smashing things together. Oh, well,

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Speaker 1: you came to the right place. I know you're a

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Speaker 1: professional smasher. I guess I'm actually wondering if it's the

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Speaker 1: right way to study things. I don't know, I mean,

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Speaker 1: what could go wrong? I mean, does it work for everything?

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Speaker 1: Like let's say you're trying out a new restaurants. Smashing

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Speaker 1: two plates together really the best way to test it?

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Speaker 1: I mean I would read that restaurant review, wouldn't you?

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Speaker 1: Or what about movies? Like you would smash Blu Ray

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Speaker 1: disc together. Maybe that's how they came up with awesome

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Speaker 1: crossover events. I mean, that's the origin of the Marvel multiverse.

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Speaker 1: Somebody had a stack of DVDs on their coffee table

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Speaker 1: and eureka, somebody smashed two comic books together, or a

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Speaker 1: comic book with a Blu Ray. There you go, that's

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Speaker 1: what happened. Smash to Hollywood actors together. Hi. I'm or Hamry,

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Speaker 1: cartoonists and the co author of Frequently Asked Questions about

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Speaker 1: the Universe. Hi, I'm Daniel. I'm a particle physicist and

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Speaker 1: a professor at U C Irvine, and I'm the other

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Speaker 1: co author of frequently asked questions about the universe. What

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Speaker 1: what a coincidence? What are the chances that we would

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Speaker 1: collide on a podcast like this? What happens when you

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Speaker 1: smash two co authors together? Do you get one big author?

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Speaker 1: You can? Do you get a voltron author? Maybe? Can

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Speaker 1: I be like left foot jokes aside? You get a

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Speaker 1: really fun book that neither of us could have written

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Speaker 1: on our own, filled with amazing physics insides, deep revelations

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Speaker 1: about the nature of the universe, and hilarious cartoons. Yeah.

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Speaker 1: It tackles really amazing and frequent questions about the universe,

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Speaker 1: like why we can't get to other stars? Or is

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Speaker 1: there an afterlife possible in this universe? Or why Daniel

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Speaker 1: doesn't believe in time travel? Wait? You don't believe in time? Terrible?

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Speaker 1: Didn't you read the book? Man, I'm gonna have to

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Speaker 1: go back in time and read it. It's too late.

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Speaker 1: You're out of time. I ran out of time, that's why.

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Speaker 1: But anyways, welcome to our podcast, Daniel and Jorge Explain

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Speaker 1: the Universe, a production of My Heart Radio in which

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Speaker 1: we smash up the two most amazing things in the universe,

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Speaker 1: your brain and the entire universe. We try to take

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Speaker 1: everything that's out there, all the craziness, the insanity, the

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Speaker 1: frothing quantum mess that is our reality, and squeeze all

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Speaker 1: of it into your brain because we believe in you.

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Speaker 1: We believe that your beautiful brain, even though with a

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Speaker 1: tiny part of the universe, can contain within it a

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Speaker 1: whole idea of the universe that we can look out

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Speaker 1: into the depths of space and actually understand what's going

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Speaker 1: on out there. On the podcast, we talk about everything

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Speaker 1: that's happening out there and explain all of it to you.

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Speaker 1: That's right. We smashed together scientific ideas and discoveries and

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Speaker 1: collide them with bad puns and a lot of conversation

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Speaker 1: here in order to pick up the pieces and hopefully

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Speaker 1: makes sense of this amazing and wonderful cosmos that we

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Speaker 1: live in. And you give me a hard time for

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Speaker 1: it sometimes, but I really do think that smashing stuff

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Speaker 1: together is really the best way to understand it. I mean, like,

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Speaker 1: who hasn't tried a sample of their neighbor's plate at

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Speaker 1: the table right and mixed it with their own dinner

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Speaker 1: to create something new? Oh? Wow? Do you ask for

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Speaker 1: their permission for us? Though? At least. I mean, usually

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Speaker 1: it's somebody in my family. So yes, I'm reaching over

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Speaker 1: to my wife's plate to try a French fry and

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Speaker 1: dip it in whatever sauces on my plate, and you

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Speaker 1: never know that could have been a culinary invention that

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Speaker 1: rocked the world. It just seems a little, you know,

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Speaker 1: sort of a destructive way of studying the universe. You know,

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Speaker 1: I'm more of an engineering type. I'd like to take

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Speaker 1: things apart, not smashing together. That's because you care about

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Speaker 1: putting them back together. I just want to know what's

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Speaker 1: going on inside. Well, I mean, doesn't it seem a

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Speaker 1: little destructive in a way, like you know, it's sort

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Speaker 1: of like a little kid which smashes things out of anger.

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Speaker 1: It is destructive, absolutely, but you know, sometimes that's all

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Speaker 1: you can do. Joking aside, If you have a toaster, yes,

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Speaker 1: you can take it apart carefully, piece by piece and

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Speaker 1: catalog what's inside it. And that probably is a better

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Speaker 1: way to understand how a toaster works than taking two

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Speaker 1: toasters and making a toaster collider. But sometimes the forces

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Speaker 1: that hold these things together are so strong and that

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Speaker 1: the only way to break it up to understand what's

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Speaker 1: going on inside is to smash it up. And that's

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Speaker 1: the case for example, with protons. But have you actually look.

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Speaker 1: Maybe there's a screwdriver for protons. You need to get

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Speaker 1: the right one with the right you know shape. Yeah,

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Speaker 1: the screw driver for protons is another proton. I guess

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Speaker 1: it's more like a hammer than a screw driver. But

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Speaker 1: then what is that screw driver made out of? Daniel? Exactly?

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Speaker 1: That's the only tool you have. If everything in the

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Speaker 1: universe is a proton, then basically you're just smashing protons together. Wait,

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Speaker 1: doesn't everything eventually fall apart or break apart? Can you

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Speaker 1: just wait for things to you know, break open? I

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Speaker 1: mean I have grand deadlines, and you know, I gotta

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Speaker 1: get stuff done. I can't just wait till the heat

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Speaker 1: death of the universe when everything collapses. I see, it's

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Speaker 1: a lack of patients, not a lack of or methods.

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Speaker 1: You're encouraging procrastination to the heat death of the universe. Right,

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Speaker 1: that's really on brand for there you go, And in

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Speaker 1: the meantime, the grant could support you. Right, that's right.

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Speaker 1: I'm going to write a grant for waiting for ten

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Speaker 1: to the fourteen years until the universe. Does it experiments

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Speaker 1: for me? We'll see how that goes. I'll cut you

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Speaker 1: and if it gets funded. Yeah, as long as it's

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Speaker 1: for ten to the fourteen dollars, I'm totally in no.

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Speaker 1: But the smashing things together does seem to be the

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Speaker 1: preferred way. Physicists like to explore things at the smallest

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Speaker 1: levels because there is no screwdriver for opening things like

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Speaker 1: protons or even courts. There is no screwdriver, there are

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Speaker 1: no tweezers, and it's something that we can actually do.

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Speaker 1: We can manipulate protons, we can tune their energy, we

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Speaker 1: can smash them together to see what's going on inside.

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Speaker 1: And the same thing is true for even bigger stuff.

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Speaker 1: We can't take stars apart. We don't have the machinery

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Speaker 1: to understand what's inside a planet, So the best way

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Speaker 1: to learn about it is to watch collisions of enormous

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Speaker 1: astronomical objects to see what's going on inside. Yeah, I

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Speaker 1: guess sometimes it's hard to take to apart, like you said, right,

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Speaker 1: Like it's hard to take a star apart. That would

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Speaker 1: be pretty difficult. It's pretty hard to take a star apart.

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Speaker 1: It's even hard to look inside a star. We had

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Speaker 1: the Parker Solar Probe recently, which came super close to

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Speaker 1: the Sun and almost fried itself but not quite. And

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Speaker 1: it gives us a picture of what's going on in

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Speaker 1: the surface and helps map a little bit of the insides.

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Speaker 1: But you know, we have questions about what's going on

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Speaker 1: deep deep in the heart of our Sun that we

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Speaker 1: could only really answer by smashing it into another star. Yeah.

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Speaker 1: I guess sometimes it's hard to look inside of the things,

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Speaker 1: so you kind of have to break them apart because

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Speaker 1: they don't open up so easily. And to be honest,

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Speaker 1: an engineer and we do sometimes match things together us

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Speaker 1: until they break. Just trust test them now, don't worry.

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Speaker 1: I don't know how to build a star collider, so

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Speaker 1: I'm not going to shoot Proximus Centauri at our star

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Speaker 1: anytime soon. That's a grand proposal that will never be funded.

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Speaker 1: But we don't have to build these colliders ourselves. We

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Speaker 1: don't have to construct cosmic colliders to smash planets together,

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Speaker 1: because the universe is doing it for us. We just

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Speaker 1: have to look out there into the skies and find

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Speaker 1: the experiment already underway. Yeah, because it is a pretty

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Speaker 1: big universe. And even though it's huge and empty. It's

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Speaker 1: pretty big and pretty full of stuff, And so there's

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Speaker 1: always something going on in the universe, and some things

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Speaker 1: that going on is a big coalition. We have seen

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Speaker 1: comets slam in the planets. We have seen binary stars

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Speaker 1: collapse into each other. We've seen all sorts of crazy

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Speaker 1: stuff smash into itself and learned an incredible amount in

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Speaker 1: the process. Yeah, we've seen galaxy smashed together, right, that's

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Speaker 1: sort of how dark matter was confirmed. Yeah, we can

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Speaker 1: see galaxies merging in the middle of this process of

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Speaker 1: swirling around each other and their stars forming one new

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Speaker 1: elliptical galaxy. And you're right, we've even seen galaxy clusters collide.

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Speaker 1: The Bullet cluster is two big groups of galaxies, enormous

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Speaker 1: piles of galaxies smashing into each other, dark matter coming

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Speaker 1: out on either side, which tells us, as you said,

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Speaker 1: the dark matter is its own thing and not just

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Speaker 1: some weird twist on gravity. Yeah. I guess smashing things

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Speaker 1: together is a good way to explore things, especially if

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Speaker 1: are sort of mysterious and kind of hard to know

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Speaker 1: that they're there or what's going on inside of them. Right,

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Speaker 1: Like smashing things with dark matter in them so it

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Speaker 1: helps you see the dark matter. Yeah, it helps you

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Speaker 1: separate the dark matter from the rest of the stuff

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Speaker 1: because different things smash differently. Right, The gas and the

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Speaker 1: dust in those galaxies smashed into each other, making huge

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Speaker 1: explosions and bright flashes of light, but the dark matter

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Speaker 1: passed right through. So that tells you that dark matter

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Speaker 1: really is different from normal kind of matter. So yeah, absolutely,

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Speaker 1: smashing stuff together a great way to figure out what's

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Speaker 1: going on, great way to support physicists. Would like to

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Speaker 1: smash things as little kids. Yeah, but you know, don't

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Speaker 1: like smash your kids together if you're not sure what

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Speaker 1: they're up to. There is a limit to this idea,

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Speaker 1: seeing well, I think they usually smash themselves pretty good

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Speaker 1: without your help or direction. All right, But in no

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Speaker 1: way am I endorsing kids smashing on the podcast. I

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Speaker 1: don't even know why you would bring it up. I

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Speaker 1: guess you know. I guess kids are mysterious. Also, they're

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Speaker 1: hard to understand. Yes, absolutely, kids are hard to understand.

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Speaker 1: But there are better ways to understand what's going on

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Speaker 1: inside your children then smashing them together, right right. I

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Speaker 1: guess you could talk to them. I guess you could

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Speaker 1: just make references to them on the podcast and hope

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Speaker 1: they listen. Yeah, maybe like twenty years from now, when

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Speaker 1: they're in therapy, they'll be like, what did my father

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Speaker 1: think of me? Oh, it's right here on this podcast.

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Speaker 1: What But anyways, there is something mysterious out there in

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Speaker 1: the universe that we would like to know more about.

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Speaker 1: We would like to know what's going on inside of him,

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Speaker 1: But so far, they are one of the hardest things

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Speaker 1: to look at and figure out. A lot of people

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Speaker 1: write to me and ask what happens when these two

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Speaker 1: mysterious objects in the universe come together? Is it just

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Speaker 1: like other collisions or are some of the fundamental rules

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Speaker 1: of the universe broken? So today on the podcast, we'll

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Speaker 1: be tackling the question what happens when black holes collide?

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Speaker 1: There's a very sensationalist question, I feel, what happens when

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Speaker 1: black holes collide. It's sort of like shark versus shark,

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Speaker 1: which shark eats the other one? You know, one black

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Speaker 1: hole sucking in the other one, these sucking each other.

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Speaker 1: What does that even mean? Man? Yeah, I know, it's

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Speaker 1: like kind of hole fall into another hole, Like, you know,

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Speaker 1: holy moly, that's a complicated question that is a whole

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Speaker 1: lot of holes there in that theory. We need a

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Speaker 1: holistic understanding of how this works. But this is sort

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Speaker 1: of part of our I guess a recent theme we've

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Speaker 1: had going on in the podcast. We can almost call

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Speaker 1: it like Smash month or smash week exactly. We got

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Speaker 1: smashing on the brain over here at the podcast headquarters.

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Speaker 1: Hopefully will be a smashing success. But we have been

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Speaker 1: smashing things together. We smashed photons together last time, and

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Speaker 1: we smashed what else do we smash? We did a

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Speaker 1: whole listener episodes question about smashing stuff together. That was

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Speaker 1: the theme annihilation questions. And then we smash light together,

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Speaker 1: which turns out you can't smash together. And now we're

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Speaker 1: smashing black holes. What's next, Danuel smashing universes? Oh wow,

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Speaker 1: universe collisions. Actually, there is a theory about different bubbles

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Speaker 1: in the multiverse and bumping into each other and leaving

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Speaker 1: an imprint on the cosmic microwave background radiation. I just

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Speaker 1: read about this theory yet. Yeah, there was a theory

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Speaker 1: by Roger Penrose, and he claimed to see evidence for

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Speaker 1: it in the cosmic microwave background radiation, but nobody could

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Speaker 1: confirm it. So it's definitely not something we've seen, but

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Speaker 1: a pretty awesome idea. Yeah. Also it's called the Big Bounce,

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Speaker 1: not the Big Smash, so we can't talk about it.

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Speaker 1: This episode sponsored by a smash Burger. But I remember

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Speaker 1: the first time I heard about black holes being collided,

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Speaker 1: and I thought, Wow, that's incredible, like two things that

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Speaker 1: we definitely do not understand. And I thought to myself,

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Speaker 1: I want to see what happens, what comes out, what's

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Speaker 1: revealed in the shards of that collision, Like, show me

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Speaker 1: the answer, universe. Yeah, what are the shards of the

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Speaker 1: two sharks when they And it's sort of amazing you

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Speaker 1: know that it happens out there in the universe and

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Speaker 1: that we can see it. So to me, it feels

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Speaker 1: like we are peaking under the rug of nature, really

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Speaker 1: understanding something deep about the nature of space and time

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Speaker 1: by looking for these extreme collisions when nature has to

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Speaker 1: tell us how things were. Because black holes are pretty

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Speaker 1: extreme in the universe, right, there's some of the most

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Speaker 1: extreme conditions imaginable. Maybe they're breaking the laws of physics inside,

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Speaker 1: or at least the laws that we didn't know, and

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Speaker 1: so you can't imagine amazing things are gonna happen when

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Speaker 1: you smash two of them together. Yeah, they're probably gonna

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Speaker 1: smash the laws of physics. And I guess maybe a

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Speaker 1: more philosophical question is, is Daniel, kid, two holes actually collide? Like, what,

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Speaker 1: what's actually hitting each other? Nothing's gonna hit each other?

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Speaker 1: Is there just two holes? I guess you could think

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Speaker 1: of them as like merging, Right, if you and a

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Speaker 1: friend are both digging holes in the ground, you just

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Speaker 1: keep digging, then eventually just get one big hole, right,

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Speaker 1: so those two holes can sort of merge. So it's

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Speaker 1: more of a black hole merger, it is. But actually

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Speaker 1: the map doesn't quite work that way because the black

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Speaker 1: hole that comes out is a little bit smaller than

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Speaker 1: the some of the two black holes that went in,

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Speaker 1: which is pretty weird. Wait what, well, you just spoiled it,

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Speaker 1: he said, Another hole comes out. I guess the two

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Speaker 1: holes don't cancel each other. Yeah, they do an amazing

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Speaker 1: dance of relativity to form something new that comes out. Well, then,

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Speaker 1: as you said, this kind of thing happens all the

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Speaker 1: time in the years, and we get to observe it, right,

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Speaker 1: we certainly do, and we learn a lot about the

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Speaker 1: nature of space and time in the process. All right, Well,

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Speaker 1: as usual, we were curious how many people out there

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Speaker 1: had heard of black holes colliding and what maybe they

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Speaker 1: think happens when they do. So thank you to everybody

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Speaker 1: who participates in these segments for our podcast. We hope

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Speaker 1: you have a good time answering random questions without any

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Speaker 1: chance to prepare. If you like to participate and hear

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Speaker 1: your speculation on the podcast for everybody else to enjoy,

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Speaker 1: please don't be shy. Right to us two questions at

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Speaker 1: Daniel and Jorge dot com. So think about it for

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Speaker 1: a second. What do you think happens when two black

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Speaker 1: holes collide? Here's what people had to say. Yeah, I

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Speaker 1: think we know this right. So if two black holes collide, hey,

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Speaker 1: they make a bigger black hole? Would be I think

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Speaker 1: some people have discovered that they make gravitational way. Put

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Speaker 1: that seems like two simple and once there. So I

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Speaker 1: read black Hole Blues by Jane Levin, and my best

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Speaker 1: guess is black holes Clyde, they circle around each other

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Speaker 1: faster and faster, and as they get um closer to

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Speaker 1: each other, they're circling almost at the speed of light.

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Speaker 1: At the very last split second, and when they Clyde.

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Speaker 1: The force has enough energy to overpower the energy that

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Speaker 1: an entire galaxy might put out, and that's why we

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Speaker 1: can sense the gravitational waves galaxies away UM here on

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Speaker 1: Earth with the new instruments we have. In general, I

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Speaker 1: don't think there's a direct collision of a black hole,

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Speaker 1: but rather they orbit each other closer and closer and closer,

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Speaker 1: with probably the stronger one feeding off of the weaker one. Ultimately,

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Speaker 1: after all the fireworks are done, I would assume that

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Speaker 1: the smaller one would be eventually absorbed into the larger one,

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Speaker 1: and you have one substantially larger black hole. When two

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Speaker 1: black holes collide, I think they just merged into a

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Speaker 1: larger one. We can observe gravitational waves happening while this occurs,

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Speaker 1: but other than that, I think they just merge. When

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Speaker 1: black holes collide, gravity waves make their way to our

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Speaker 1: clever listening devices here on Earth and UM I think

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Speaker 1: probably is a lot of energy released and they become

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Speaker 1: one black hole. When black holes collide, I mean you

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Speaker 1: have very very heavy, heavily dense, and very strong gravity

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Speaker 1: come from these things. So when they collide, it's got

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Speaker 1: a kind of one window which everyone is a more

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Speaker 1: dense and be strongly have stronger gravitational forces, and then

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Speaker 1: it's kind of absorbs. They make a lot of gravity

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Speaker 1: waves and then they make one big all right, A

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Speaker 1: lot of fun answers here. I like the one that

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Speaker 1: said when they collide they eat each other kind of

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Speaker 1: like sharks. But who is eating who? Man, that doesn't really.

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Speaker 1: But if one shark starts eating the tail of the

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Speaker 1: other shark, and then the other shark starts eating tail

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Speaker 1: the other shark, what's going to happen? It's like a

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Speaker 1: yin yang shark somehow, Yeah, ying shark. Yeah, maybe the

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Speaker 1: shark ends up eating itself when you get a sharknado

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Speaker 1: because they're spinning around so fast. That's probably how that

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Speaker 1: crossover event happened, right, A Shark DVD and a Tornado DVD. Boom?

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Speaker 1: That's right. Yeah, one bad idea smashed another bad idea. Yeah,

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Speaker 1: why not? Right? Who knows what happens when you collide

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Speaker 1: the craziest things in the universe. So I love the

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Speaker 1: creativity there, thank you? Yeah, why not? Maybe that should

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Speaker 1: be the hell of the podcast. Why not, let's get smashing. Well,

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Speaker 1: let's break it down for people here. Daniel maybe let's

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Speaker 1: start with the basics. What is a black hole. Black hole,

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Speaker 1: as you said, is a hole in space and time,

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Speaker 1: but it is a really strange hole, you know. Really,

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Speaker 1: what it is is a location where there's so much

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Speaker 1: mass and energy in one spot that's it's dense enough

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Speaker 1: that particles that are near it are doomed to fall in.

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Speaker 1: You know, mass and energy hells space how to bend,

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Speaker 1: and then space tells and particles and mass and other

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Speaker 1: things how to move. So the more mass and energy

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Speaker 1: you have somewhere, the more space curve, which is why,

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Speaker 1: for example satellites or with the Earth instead of just

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Speaker 1: flying away, you could think of all of gravity in

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Speaker 1: fact as the invisible curvature of space rather than like

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Speaker 1: a Newtonian tugging. And so black holes are where space

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Speaker 1: is curved so much that there are particles that can

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Speaker 1: never escape. So there's sort of holes in space, and

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Speaker 1: there's sort of holes caused by gravity, right, Like that's

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Speaker 1: another way to do sort of think about at it, right,

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Speaker 1: And it's it's like there's there's so much stuff and

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Speaker 1: energy in them that it just sucks everything in and

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Speaker 1: and it sucks them so much you can never get

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Speaker 1: up Yeah. Mostly you can think about gravity in two

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Speaker 1: different ways. You can think about like a force something

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Speaker 1: is pulling on you, and like the Earth is tugging

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Speaker 1: on you. That sort of Newton's idea of gravity. But

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Speaker 1: black holes come out of general relativity, which encouras you

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Speaker 1: to think about gravity in a very different way, since

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Speaker 1: the gravity isn't a force, it's just that space is curved.

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Speaker 1: But you can't see that curvature. The only thing you

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Speaker 1: can see is the effect of that curvature on the

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Speaker 1: motion of objects. So you shine a flashlight, for example,

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Speaker 1: through curved space, then it seems to you to bend,

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Speaker 1: but that bending is just because it's moving in a

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Speaker 1: straight line through curved space you can't see. So when

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Speaker 1: you apply that to black holes, you don't get like

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Speaker 1: a really strong force of gravity. You at a place

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Speaker 1: where space has ben so much that now it's just

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Speaker 1: one directional Things inside the event of horizon of a

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Speaker 1: black hole always end up at the singularity, according to

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Speaker 1: general relativity, because that's the only direction left in space.

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Speaker 1: Right Yeah, But general relativity might be wrong to right, Like,

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Speaker 1: there's this possibility that maybe gravity is a forcedome. There

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Speaker 1: are forests, gravity particles, and everything right. General relativity almost

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Speaker 1: certainly wrong at some level, not in the sense that

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Speaker 1: it's making mistakes about GPS or that we're getting the

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Speaker 1: numbers wrong, but it can't really be the true description

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Speaker 1: of nature, as you said, because, for example, it predicts

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Speaker 1: singularities at the hearts of black hole, and you know

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Speaker 1: that's not as much a physical prediction like general relativity is,

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Speaker 1: and say there is a point of infinite density as

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Speaker 1: much as it's a breakdown of the theory. It says, well,

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Speaker 1: here's what I predict, and that seems sort of nonsense,

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Speaker 1: so at this point, replace me with a better theory.

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Speaker 1: So we don't know what's going on at the heart

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Speaker 1: of black holes. It could be that the right picture

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Speaker 1: of gravity is as a sort of quantum field. The

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Speaker 1: way we have all the other forces. You can think

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Speaker 1: about gravity is the exchange of gravitons. So yeah, you're right,

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Speaker 1: general relativity almost certainly wrong. On the other hand, it

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Speaker 1: predicts black holes and we see them, so it's right

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Speaker 1: about a lot of stuff. Well, black holes are really strange,

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Speaker 1: and there are a couple of really strange things about them, Like,

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Speaker 1: first of all, I like can't escape, so they just

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Speaker 1: look like a giant whole and space, but it also

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Speaker 1: does interesting things like slow down time. Yeah, there are

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Speaker 1: two different kinds of time dilation in our universe from relativity.

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Speaker 1: One is much more commonly talked about, which is velocity

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Speaker 1: based time dilation. If you see somebody moving fast through

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Speaker 1: the universe relative to you, you see their clocks slowing down,

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Speaker 1: And that kind of time dilation is relative because if

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Speaker 1: they look back at you, they see your clocks slowing down.

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Speaker 1: So you too, disagree about whose clock is slowing down,

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Speaker 1: which is really weird and confusing makes you doubt like

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Speaker 1: you know, truth and the existence of reality. But the

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Speaker 1: kind of time dilation that happens to a black hole

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Speaker 1: is different. The more space is curved where you are,

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Speaker 1: the more your clock will slow down. And that's not

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Speaker 1: a relative effect, is absolute. So if your friend gets

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Speaker 1: near a black hole where space is curved more, you

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Speaker 1: will see their clocks slow down because they're in more

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Speaker 1: curved space. They will see your clock going faster. Right,

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Speaker 1: it's the opposite of the relative time dilation that happens

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Speaker 1: due to velocity. Here is absolutely because everybody agrees. So

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Speaker 1: if you are falling near a black hole, your friend

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Speaker 1: will see you slow down, and you will see them

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Speaker 1: sped up. Yet it's pretty cool effect. And like you

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Speaker 1: will literally see them moving slow motion, right, and they

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Speaker 1: will literally see the entire rest of the universe moving

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Speaker 1: in fast forward. Yeah. And so if you see somebody

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Speaker 1: falling towards the black hole, the closer they get, the

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Speaker 1: more their time slows down. And so it actually takes

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Speaker 1: an infinite amount of time for the last thing to

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Speaker 1: fall into a black hole. Like you toss the banana

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Speaker 1: into a black hole, you don't actually see it enter

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Speaker 1: the black hole past the event horizon until time equals infinity. Right.

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Speaker 1: We've had I think whole podcast about this because it's

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Speaker 1: it's sort of a little bit mind bending because you

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Speaker 1: do sort of see black holes growing over time, right,

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Speaker 1: and at some point that they're going to overtake the banana. Right. Yeah,

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Speaker 1: that seems confusing because it suggests the black holes could

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Speaker 1: never grow because nothing could actually fall into them. That's

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Speaker 1: why I said it's only true for the last thing

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Speaker 1: to fall into a black hole because as the banana

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Speaker 1: falls towards the black hole, the event horizon actually grows

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Speaker 1: before the banana crosses over. A black hole isn't like

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Speaker 1: a pet where you need to put something in it

427
00:22:09,720 --> 00:22:11,320
Speaker 1: for it to get bigger, doesn't have to like eat

428
00:22:11,359 --> 00:22:14,119
Speaker 1: the banana the sides. The event horizon reflects the total

429
00:22:14,160 --> 00:22:17,280
Speaker 1: gravitational energy of the system. So as the banana falls

430
00:22:17,280 --> 00:22:19,840
Speaker 1: into the black hole, the event horizon actually grows out

431
00:22:19,960 --> 00:22:21,720
Speaker 1: to meet it. And then if you throw something else

432
00:22:21,760 --> 00:22:24,960
Speaker 1: like an apple after the banana, that also pulls out

433
00:22:25,000 --> 00:22:27,880
Speaker 1: the event horizon, so it will come and encompass the banana.

434
00:22:28,080 --> 00:22:30,320
Speaker 1: So that's how we see black holes actually grow out

435
00:22:30,320 --> 00:22:32,840
Speaker 1: there in the universe is a continuous stream of stuff

436
00:22:33,040 --> 00:22:36,040
Speaker 1: falling into it and pulling out the event horizon. Right,

437
00:22:36,080 --> 00:22:37,840
Speaker 1: But you don't have to feed them, but it's it's

438
00:22:37,960 --> 00:22:39,640
Speaker 1: nice to feed them, right. You don't want a black

439
00:22:39,640 --> 00:22:42,879
Speaker 1: hole to starve. I don't know. It depends where the

440
00:22:42,880 --> 00:22:44,639
Speaker 1: black hole lives. If it lives in your basement, I

441
00:22:44,640 --> 00:22:46,800
Speaker 1: don't think it's a good idea to feed it. I

442
00:22:46,880 --> 00:22:48,640
Speaker 1: think if it lives up in your basement, it's game

443
00:22:48,720 --> 00:22:52,040
Speaker 1: over for you for here house. You know, there is

444
00:22:52,160 --> 00:22:55,919
Speaker 1: some size of a black hole where it's radiating away energy,

445
00:22:56,040 --> 00:22:57,840
Speaker 1: and you could feed it at the same rate, so

446
00:22:57,880 --> 00:22:59,840
Speaker 1: you could have a stable black hole that you keep

447
00:23:00,160 --> 00:23:03,600
Speaker 1: pet You can't have a pet then you just contradicted yourself.

448
00:23:03,760 --> 00:23:05,480
Speaker 1: Just don't pet it. I guess you don't touch it.

449
00:23:06,040 --> 00:23:09,040
Speaker 1: I wouldn't recommend it. But theoretically it's possible to keep

450
00:23:09,040 --> 00:23:11,400
Speaker 1: a black hole stable. I see. And so something else

451
00:23:11,440 --> 00:23:13,800
Speaker 1: that's interesting about a black hole is that there are

452
00:23:13,800 --> 00:23:15,720
Speaker 1: only a few things we can know about them, right,

453
00:23:15,760 --> 00:23:17,919
Speaker 1: I mean, they're a black hole. Stuff falls in and

454
00:23:17,920 --> 00:23:19,760
Speaker 1: we never see it again, but there are a few

455
00:23:19,760 --> 00:23:22,320
Speaker 1: things that you can tell about them. Everything that falls

456
00:23:22,359 --> 00:23:24,240
Speaker 1: into the event horizon is lost to us and what

457
00:23:24,359 --> 00:23:27,560
Speaker 1: happens to it, and we cannot know information about what's

458
00:23:27,560 --> 00:23:30,920
Speaker 1: inside the event horizon. Can't escape. But that doesn't mean

459
00:23:30,920 --> 00:23:33,840
Speaker 1: we can't measure things about the global black hole. Like

460
00:23:33,880 --> 00:23:36,520
Speaker 1: a black hole has mass, It tugs on you even

461
00:23:36,520 --> 00:23:39,320
Speaker 1: though you're outside the event horizon, and so you can

462
00:23:39,440 --> 00:23:42,199
Speaker 1: use that to measure how much stuff is inside the

463
00:23:42,200 --> 00:23:44,760
Speaker 1: event horizon. How much mass does this black hole have.

464
00:23:45,320 --> 00:23:47,320
Speaker 1: So there are a few things you can measure from

465
00:23:47,359 --> 00:23:50,359
Speaker 1: outside the event horizon, and that's the mass of the

466
00:23:50,359 --> 00:23:53,760
Speaker 1: black hole. Also the electric charge of the black hole,

467
00:23:53,840 --> 00:23:56,239
Speaker 1: because charge is conserved in the universe. You drop an

468
00:23:56,240 --> 00:23:58,919
Speaker 1: electron into a black hole that changes its charge and

469
00:23:59,000 --> 00:24:02,440
Speaker 1: its electric yield. The same thing for its spin. Black

470
00:24:02,480 --> 00:24:04,840
Speaker 1: holes can spin. So there's this theorem called the no

471
00:24:05,119 --> 00:24:08,000
Speaker 1: hair theorem that says those the only three things you

472
00:24:08,040 --> 00:24:12,640
Speaker 1: can know about a stable black hole, mass, spin, and charge. Wait,

473
00:24:12,640 --> 00:24:14,919
Speaker 1: what is it called the no hair theorem? How does

474
00:24:15,000 --> 00:24:18,040
Speaker 1: hair falling get fit into this? I think it's a

475
00:24:18,119 --> 00:24:20,679
Speaker 1: joke that says that you can't know whether black holes

476
00:24:20,720 --> 00:24:23,399
Speaker 1: are hairy, Like you can't know what's going on inside

477
00:24:23,440 --> 00:24:26,040
Speaker 1: the black hole that have blonde hairs, have a mohawk.

478
00:24:26,440 --> 00:24:28,600
Speaker 1: It's like, you know, just an example of something you

479
00:24:28,640 --> 00:24:31,760
Speaker 1: can't know about a black hole. M it could have

480
00:24:31,800 --> 00:24:34,640
Speaker 1: been called the no tattoos theorem. Also, yeah, that makes

481
00:24:34,640 --> 00:24:37,959
Speaker 1: no sense to me, but that's the official name. All right,

482
00:24:38,000 --> 00:24:40,120
Speaker 1: Well that's a black hole. And so now the big

483
00:24:40,200 --> 00:24:43,080
Speaker 1: question is what happens if I take two black holes

484
00:24:43,160 --> 00:24:46,960
Speaker 1: and I smushed them or smashed them or merged them together.

485
00:24:47,720 --> 00:24:49,959
Speaker 1: Apparently a lot of things happen. So let's get into that.

486
00:24:50,000 --> 00:25:05,160
Speaker 1: But first let's take a quick break. Alright, we're talking

487
00:25:05,200 --> 00:25:09,119
Speaker 1: about smashing black holes together, and Daniel, this happens all

488
00:25:09,119 --> 00:25:12,080
Speaker 1: the time, right, Like we've recently been able to listen

489
00:25:12,119 --> 00:25:14,800
Speaker 1: to black holes colliding, and a lot of they had.

490
00:25:14,840 --> 00:25:16,600
Speaker 1: They happened more often than we thought in black hole

491
00:25:16,640 --> 00:25:20,119
Speaker 1: collisions were first observed in two thousand and fifteen, but

492
00:25:20,160 --> 00:25:23,040
Speaker 1: it was a very, very long search for black holes.

493
00:25:23,119 --> 00:25:26,240
Speaker 1: People started decades and decades before that trying to invent

494
00:25:26,320 --> 00:25:30,320
Speaker 1: systems that were sensitive enough to the radiation emitted from

495
00:25:30,320 --> 00:25:32,920
Speaker 1: black hole collisions so that we could see it here

496
00:25:33,000 --> 00:25:36,040
Speaker 1: on Earth. This is something predicted by Albert Einstein, though

497
00:25:36,080 --> 00:25:38,600
Speaker 1: he thought we could never actually observe it, that this

498
00:25:38,640 --> 00:25:41,479
Speaker 1: is a cool effect. Too bad, it's too tiny for

499
00:25:41,560 --> 00:25:43,879
Speaker 1: us to ever see. Oh I see, so before we

500
00:25:43,960 --> 00:25:47,160
Speaker 1: could listen to them with gravitational waves. People were trying

501
00:25:47,200 --> 00:25:49,800
Speaker 1: to see them, but they never found any right, Yeah,

502
00:25:49,800 --> 00:25:51,920
Speaker 1: people were trying to listen to them with gravitational waves

503
00:25:51,920 --> 00:25:54,040
Speaker 1: for a long time. That was Einstein's prediction that they

504
00:25:54,040 --> 00:25:57,040
Speaker 1: would create from gravitational waves, but it would be impossible

505
00:25:57,080 --> 00:25:59,800
Speaker 1: for us to see these gravitational waves to observe them.

506
00:26:00,000 --> 00:26:01,720
Speaker 1: And you know, I'm in the company who agreed with

507
00:26:01,720 --> 00:26:03,800
Speaker 1: Einstein for a long time. When I was thinking about

508
00:26:03,880 --> 00:26:06,400
Speaker 1: grad school, I had a few different choices, and one

509
00:26:06,480 --> 00:26:09,399
Speaker 1: was going to university that was deep into ligo, that

510
00:26:09,480 --> 00:26:12,959
Speaker 1: was developing the technology and trying to observe gravitational waves,

511
00:26:13,080 --> 00:26:15,679
Speaker 1: and I remember thinking, that's cool, but they're never going

512
00:26:15,720 --> 00:26:17,720
Speaker 1: to make that happen, and so I'm gonna go do

513
00:26:17,800 --> 00:26:20,800
Speaker 1: particle because instead. Yeah, yeah, I'm in the company of

514
00:26:20,800 --> 00:26:24,639
Speaker 1: Einstein as well. I have crazy hair as well. But

515
00:26:24,760 --> 00:26:27,680
Speaker 1: Einstein was wrong and so was I, because they did

516
00:26:27,760 --> 00:26:30,720
Speaker 1: see gravitational waves. They did see this crazy pattern of

517
00:26:30,800 --> 00:26:34,440
Speaker 1: radiation emitted from the collisions of black holes. Yeah, I

518
00:26:34,480 --> 00:26:37,200
Speaker 1: think what I was asking is, like, could you see

519
00:26:37,240 --> 00:26:40,000
Speaker 1: two black holes merging together? I mean, we can sort

520
00:26:40,000 --> 00:26:42,639
Speaker 1: of see black holes out there in the universe, and

521
00:26:42,640 --> 00:26:45,520
Speaker 1: we can definitely see their effect on the stars or

522
00:26:45,560 --> 00:26:48,639
Speaker 1: the galaxy around them. Could you ever hope to, you know,

523
00:26:48,720 --> 00:26:52,560
Speaker 1: detect the black hole collision without the gravitational waves tection, Like,

524
00:26:52,600 --> 00:26:55,520
Speaker 1: could you ever see two black holes actually colliding? You

525
00:26:55,560 --> 00:26:57,840
Speaker 1: can't actually see them, but you're right, you don't see

526
00:26:57,840 --> 00:27:01,400
Speaker 1: the black holes themselves colliding. Black holes are surrounded by

527
00:27:01,400 --> 00:27:03,760
Speaker 1: accretion disks, all sorts of matter that sort of on

528
00:27:03,920 --> 00:27:07,240
Speaker 1: deck for falling into the black holes, and so sometimes

529
00:27:07,240 --> 00:27:10,280
Speaker 1: when two black holes collide, there are creation discs also

530
00:27:10,359 --> 00:27:13,320
Speaker 1: collide and create light. They've seen as a couple of

531
00:27:13,320 --> 00:27:16,439
Speaker 1: times where they've seen flashes of bright light at the

532
00:27:16,480 --> 00:27:19,200
Speaker 1: same time and in the same direction as they've observed

533
00:27:19,200 --> 00:27:22,280
Speaker 1: gravitational waves. So they have seen in a couple of

534
00:27:22,280 --> 00:27:27,000
Speaker 1: occasions bright flashes of light emitted from black hole collisions. Right,

535
00:27:27,040 --> 00:27:30,359
Speaker 1: but before like maybe you would see the bright flash

536
00:27:30,400 --> 00:27:32,600
Speaker 1: of light, but you wouldn't be able to know if

537
00:27:32,640 --> 00:27:35,679
Speaker 1: it was a black hole collision. Yeah, exactly, it just

538
00:27:35,720 --> 00:27:37,399
Speaker 1: seemed like a flash of light. And there's lots of

539
00:27:37,400 --> 00:27:40,320
Speaker 1: weird flashes of light in the universe and you can't

540
00:27:40,320 --> 00:27:42,879
Speaker 1: necessarily tell that one is from a black hole or

541
00:27:43,000 --> 00:27:45,440
Speaker 1: from something else, or just from two stars colliding or

542
00:27:45,440 --> 00:27:48,800
Speaker 1: two blobs of gas colliding. So really, the unique signature

543
00:27:48,840 --> 00:27:50,239
Speaker 1: and the thing that told us that black holes were

544
00:27:50,240 --> 00:27:53,719
Speaker 1: colliding where these patterns of gravitational waves, which are like

545
00:27:53,880 --> 00:27:57,520
Speaker 1: ripples in space and time itself. And so far since

546
00:27:58,280 --> 00:28:00,919
Speaker 1: we've seen a whole bunch of I've heard a but

547
00:28:01,000 --> 00:28:03,800
Speaker 1: a whole bunch of these black hole collisions, like maybe

548
00:28:03,880 --> 00:28:06,359
Speaker 1: like ten a year or something. Right, it's incredible we

549
00:28:06,400 --> 00:28:08,920
Speaker 1: have like fifty examples now and to appreciate how amazing

550
00:28:08,960 --> 00:28:11,920
Speaker 1: that is, realized that we didn't know how often black

551
00:28:11,920 --> 00:28:15,080
Speaker 1: holes collided. When Lego turned on, it was like a

552
00:28:15,119 --> 00:28:17,920
Speaker 1: new kind of instrument, and we're listening to something new

553
00:28:17,960 --> 00:28:19,760
Speaker 1: in the universe, or a new kind of eyeball. We're

554
00:28:19,760 --> 00:28:21,720
Speaker 1: looking for things in the universe. It's all just an

555
00:28:21,760 --> 00:28:24,680
Speaker 1: analogy because gravitational radiation is not something you can see

556
00:28:25,040 --> 00:28:27,520
Speaker 1: or here. We're just trying to translated into sort of

557
00:28:27,600 --> 00:28:29,840
Speaker 1: human experience. But we didn't know if this kind of

558
00:28:29,840 --> 00:28:32,879
Speaker 1: thing happened once in a century, once in a millennium,

559
00:28:33,240 --> 00:28:35,680
Speaker 1: or like ten times a second. So when they turned

560
00:28:35,720 --> 00:28:37,160
Speaker 1: this thing on, it could have been that they were

561
00:28:37,160 --> 00:28:40,120
Speaker 1: waiting for years to hear the first one, or that

562
00:28:40,200 --> 00:28:43,320
Speaker 1: they came fast and hard and amazingly. We were lucky,

563
00:28:43,400 --> 00:28:46,320
Speaker 1: and they're pretty common. And they saw a gravitational wave

564
00:28:46,560 --> 00:28:49,160
Speaker 1: in the first test run, Like they turned this thing

565
00:28:49,200 --> 00:28:51,400
Speaker 1: on and they were just like doing calibration runs just

566
00:28:51,440 --> 00:28:54,120
Speaker 1: to make sure everything was working, and boom, they saw

567
00:28:54,120 --> 00:28:57,120
Speaker 1: a signal in the first calibration run. So they were

568
00:28:57,120 --> 00:28:59,600
Speaker 1: like off to the races, writing a paper and week two.

569
00:29:00,120 --> 00:29:03,080
Speaker 1: It's pretty amazing, pretty cool, And they happen pretty often,

570
00:29:03,080 --> 00:29:05,400
Speaker 1: maybe like once a month, once every month and a half.

571
00:29:05,440 --> 00:29:07,640
Speaker 1: And do they happen here in our galaxy, or are

572
00:29:07,680 --> 00:29:10,560
Speaker 1: we listening to these collisions from all over the universe.

573
00:29:10,720 --> 00:29:12,920
Speaker 1: They happen all over the universe, and we can see

574
00:29:12,960 --> 00:29:15,880
Speaker 1: these things really far away, like billions of light years. Now,

575
00:29:15,880 --> 00:29:18,440
Speaker 1: the further you are away from these things, of course,

576
00:29:18,480 --> 00:29:21,520
Speaker 1: the fainter they are, and so they're closer, is easier

577
00:29:21,560 --> 00:29:23,880
Speaker 1: for us to see them there, further away than the

578
00:29:23,960 --> 00:29:27,080
Speaker 1: head needs to be more dramatic, more powerful for us

579
00:29:27,080 --> 00:29:30,600
Speaker 1: to observe them. But we've detected these collisions from black

580
00:29:30,600 --> 00:29:33,560
Speaker 1: holes that are billions of light years away, But are

581
00:29:33,600 --> 00:29:36,360
Speaker 1: they happening here in our milk away galaxy? We see

582
00:29:36,360 --> 00:29:39,120
Speaker 1: black hole collisions fairly commonly, but we can see them

583
00:29:39,120 --> 00:29:42,160
Speaker 1: from really really far away, and they don't happen actually

584
00:29:42,160 --> 00:29:45,600
Speaker 1: that often in any individual galaxy, so we haven't actually

585
00:29:45,600 --> 00:29:48,400
Speaker 1: seen one happen yet in the Milky Way. Remember, the

586
00:29:48,440 --> 00:29:50,640
Speaker 1: black holes are not that common. We have really big

587
00:29:50,680 --> 00:29:53,280
Speaker 1: ones in the center of the galaxy, the black holes

588
00:29:53,600 --> 00:29:56,640
Speaker 1: created from stellar collapse. But they get two black holes

589
00:29:56,640 --> 00:29:58,680
Speaker 1: to collide. You really need like two black holes in

590
00:29:58,680 --> 00:30:01,440
Speaker 1: a binary system, because I guess it fifty seems like

591
00:30:01,480 --> 00:30:04,560
Speaker 1: a lot of black holes colliding. But it's a big universe, right,

592
00:30:04,560 --> 00:30:06,840
Speaker 1: there are trillions of galaxies out there, so the fact

593
00:30:06,880 --> 00:30:10,120
Speaker 1: that we're only seeing you know, maybe one year, it

594
00:30:10,320 --> 00:30:13,600
Speaker 1: means that maybe they're not that common. Yeah, they're not

595
00:30:13,640 --> 00:30:16,000
Speaker 1: that common sort of per galaxy, but they happen often

596
00:30:16,120 --> 00:30:18,440
Speaker 1: enough for us to have a pretty nice data sample,

597
00:30:18,760 --> 00:30:20,680
Speaker 1: which means that we can really study these things. It's

598
00:30:20,720 --> 00:30:23,160
Speaker 1: not just like we saw one and then we're wondering

599
00:30:23,200 --> 00:30:25,520
Speaker 1: if that was typical or not. We have like dozens

600
00:30:25,600 --> 00:30:27,960
Speaker 1: of these things, so we can start to ask statistical

601
00:30:28,080 --> 00:30:30,840
Speaker 1: questions about what's likely and what's common. We can see

602
00:30:30,840 --> 00:30:33,040
Speaker 1: which ones are weird, which ones are normal. It's really

603
00:30:33,080 --> 00:30:34,760
Speaker 1: an awesome moment when you can start to do like

604
00:30:34,920 --> 00:30:40,280
Speaker 1: population science on black hole collisions. Yeah, like statistical you

605
00:30:40,320 --> 00:30:43,480
Speaker 1: know surveys. All right, Well, maybe step us through here.

606
00:30:43,640 --> 00:30:46,840
Speaker 1: What happens? What's like, step by step, what's going on

607
00:30:46,920 --> 00:30:49,520
Speaker 1: when two black holes collide? Because you know, I think

608
00:30:49,560 --> 00:30:51,080
Speaker 1: one thing that a lot of people might not know

609
00:30:51,160 --> 00:30:53,120
Speaker 1: is that black holes can move, right, Like it's fair

610
00:30:53,200 --> 00:30:54,880
Speaker 1: to think of a whole moving like a hole in

611
00:30:54,880 --> 00:30:57,280
Speaker 1: the ground doesn't move, but black holes can move when

612
00:30:57,280 --> 00:31:00,080
Speaker 1: they can sort of like fly through space and and

613
00:31:00,160 --> 00:31:02,440
Speaker 1: run into other black holes. You know, black holes have

614
00:31:02,680 --> 00:31:05,120
Speaker 1: bass just like everything else, and so they have inertia

615
00:31:05,160 --> 00:31:07,800
Speaker 1: and they can have momentum. Black hole can move in

616
00:31:07,840 --> 00:31:10,080
Speaker 1: the same way that you can move past a black hole.

617
00:31:10,280 --> 00:31:13,400
Speaker 1: Remember that velocity is just relative in our universe. So

618
00:31:13,520 --> 00:31:15,840
Speaker 1: if you're flying past the black hole from its point

619
00:31:15,840 --> 00:31:17,360
Speaker 1: of view, then from your point of view, the black

620
00:31:17,400 --> 00:31:20,680
Speaker 1: hole is flying past you, right, And so these things

621
00:31:20,680 --> 00:31:23,040
Speaker 1: definitely can move. And a lot of people probably think

622
00:31:23,040 --> 00:31:26,200
Speaker 1: about black hole collisions like two black holes just flying

623
00:31:26,200 --> 00:31:28,960
Speaker 1: through space and bumping into each other like two dogs

624
00:31:28,960 --> 00:31:31,200
Speaker 1: in the park smashing into each other or something, because

625
00:31:31,240 --> 00:31:33,880
Speaker 1: they weren't looking where they were going. Instead, these two

626
00:31:33,920 --> 00:31:37,560
Speaker 1: things have sort of been faded to collide since their birth.

627
00:31:38,000 --> 00:31:41,600
Speaker 1: Remember that a lot of stars are born as binary systems.

628
00:31:41,640 --> 00:31:44,520
Speaker 1: They were made near each other and gravitationally bound from

629
00:31:44,520 --> 00:31:47,400
Speaker 1: the beginning, orbiting each other in a long dance, and

630
00:31:47,440 --> 00:31:50,080
Speaker 1: that's how most black hole collisions happen. They start as

631
00:31:50,080 --> 00:31:53,040
Speaker 1: a binary star system, then each one collapses into a

632
00:31:53,080 --> 00:31:55,680
Speaker 1: black hole. Then you get black holes orbiting each other.

633
00:31:55,960 --> 00:31:57,960
Speaker 1: So they've always been neighbors. It's not like they're just

634
00:31:58,000 --> 00:32:00,760
Speaker 1: two strangers that smash into each other and they're obitting

635
00:32:00,800 --> 00:32:05,000
Speaker 1: each other and they're slowly losing that energy, radiating away

636
00:32:05,320 --> 00:32:10,120
Speaker 1: their orbital energy until eventually they collide. WHOA, yeah, because

637
00:32:10,160 --> 00:32:13,240
Speaker 1: I guess most black holes come from stars. And so

638
00:32:13,280 --> 00:32:16,120
Speaker 1: if you have a binary system and both stars turn

639
00:32:16,200 --> 00:32:18,040
Speaker 1: into a black hole, then you have a binary black

640
00:32:18,080 --> 00:32:20,880
Speaker 1: hole system. Right, But isn't that sort of rare? I mean,

641
00:32:20,880 --> 00:32:22,920
Speaker 1: it's a little rare first start to turn into a

642
00:32:22,920 --> 00:32:25,600
Speaker 1: black hole. But now yet you need to have both

643
00:32:25,600 --> 00:32:27,840
Speaker 1: of them in the binary star system turned into black

644
00:32:27,880 --> 00:32:30,440
Speaker 1: holes exactly. And so those are the conditions you need.

645
00:32:30,920 --> 00:32:33,640
Speaker 1: And we're still understanding your black hole formation. But it

646
00:32:33,680 --> 00:32:36,960
Speaker 1: depends on how much mass there was in each individual star.

647
00:32:37,360 --> 00:32:40,080
Speaker 1: If it's a massive enough, then eventually it will collapse

648
00:32:40,200 --> 00:32:42,240
Speaker 1: into a black hole. There's like no way to avoid

649
00:32:42,280 --> 00:32:44,320
Speaker 1: it when it burns up its fuel. And the thing

650
00:32:44,360 --> 00:32:47,720
Speaker 1: I think is interesting is understanding why these things are inevitable,

651
00:32:47,720 --> 00:32:49,960
Speaker 1: Like why can't two black holes just orbit each other

652
00:32:50,080 --> 00:32:52,640
Speaker 1: happily forever until the end of the universe. Why do

653
00:32:52,720 --> 00:32:55,440
Speaker 1: they have to fall into each other? Right? Like in

654
00:32:55,480 --> 00:32:58,800
Speaker 1: our solar system, you know, are the planets are orbiting

655
00:32:58,840 --> 00:33:02,120
Speaker 1: the Sun pretty stably, pretty stable, e that's true, We're

656
00:33:02,120 --> 00:33:05,360
Speaker 1: not falling to the Sun yet, not today and not tomorrow.

657
00:33:05,720 --> 00:33:08,640
Speaker 1: But you know, these orbits are not technically stable because

658
00:33:08,680 --> 00:33:11,760
Speaker 1: every time you're in orbit around something, you're accelerating, and

659
00:33:11,880 --> 00:33:15,560
Speaker 1: anything that's accelerating in our universe, it's changing its velocity,

660
00:33:15,920 --> 00:33:20,560
Speaker 1: is generating gravitational waves. You know what is a gravitational wave.

661
00:33:20,600 --> 00:33:24,080
Speaker 1: It's just when your gravitational field changes. If you have

662
00:33:24,160 --> 00:33:27,560
Speaker 1: an object in space, it has a gravitational field, it's

663
00:33:27,640 --> 00:33:31,200
Speaker 1: changing the shape the curvature of space. Is that object accelerates,

664
00:33:31,280 --> 00:33:35,000
Speaker 1: then the curvature of space changes, but it doesn't change instantaneously.

665
00:33:35,200 --> 00:33:37,560
Speaker 1: Just like if the Sun disappeared, we wouldn't notice for

666
00:33:37,640 --> 00:33:39,840
Speaker 1: eight minutes or whatever. It would take time for that

667
00:33:39,920 --> 00:33:44,400
Speaker 1: gravitational information to propagate. And so when something accelerates, it's

668
00:33:44,480 --> 00:33:47,440
Speaker 1: changing the curvature of space, and that's what's happening when

669
00:33:47,440 --> 00:33:50,320
Speaker 1: the Earth is going around the Sun. It's accelerating and

670
00:33:50,360 --> 00:33:53,160
Speaker 1: so that radiates away some energy in terms of the

671
00:33:53,280 --> 00:33:57,240
Speaker 1: information about updating the curvature, right right, So we're slowly

672
00:33:57,240 --> 00:33:59,720
Speaker 1: losing a little bit of energy in our orbit and

673
00:33:59,760 --> 00:34:03,040
Speaker 1: so eventually, I guess in the very very very very

674
00:34:03,080 --> 00:34:06,160
Speaker 1: far future, the Earth is gonna fall into the Sun.

675
00:34:06,360 --> 00:34:09,080
Speaker 1: That's right, although other things will happen before the Earth

676
00:34:09,120 --> 00:34:12,200
Speaker 1: falls into the Sun due to radiating gravitational energy because

677
00:34:12,200 --> 00:34:14,200
Speaker 1: the Earth is not that massive. But if you have

678
00:34:14,280 --> 00:34:17,120
Speaker 1: two black holes that are really really massive, they're going

679
00:34:17,160 --> 00:34:20,319
Speaker 1: to radiate a lot more gravitational energy, and so as

680
00:34:20,320 --> 00:34:23,520
Speaker 1: they lose energy, they fall into each other. Right. They

681
00:34:23,560 --> 00:34:26,280
Speaker 1: can't maintain their orbit if they don't have that energy,

682
00:34:26,480 --> 00:34:28,920
Speaker 1: so they're very orbit The thing that's accelerating them around

683
00:34:28,920 --> 00:34:32,359
Speaker 1: each other is shaking the curvature of space around them,

684
00:34:32,400 --> 00:34:35,880
Speaker 1: creating these gravitational waves and forcing them to get closer

685
00:34:35,920 --> 00:34:39,200
Speaker 1: and closer and faster and faster, so it's more like

686
00:34:39,239 --> 00:34:42,239
Speaker 1: a swirl in than a collision. Right. It's sort of

687
00:34:42,280 --> 00:34:45,120
Speaker 1: like if you have a still lake or a still

688
00:34:45,120 --> 00:34:47,160
Speaker 1: body of water and you take two fingers and you

689
00:34:47,200 --> 00:34:49,600
Speaker 1: sort of rotate them or spin them around each other,

690
00:34:49,760 --> 00:34:53,080
Speaker 1: they're gonna be generating waves on the water. That's sort

691
00:34:53,080 --> 00:34:55,840
Speaker 1: of how people see the two black holes, kind of

692
00:34:55,960 --> 00:34:59,239
Speaker 1: radiating out energy as waves exactly. And it's a deep

693
00:34:59,280 --> 00:35:03,040
Speaker 1: concept that's really applicable to lots of different physical phenomena, right,

694
00:35:03,120 --> 00:35:06,719
Speaker 1: Like how do you generate radio transmissions? You take electrons,

695
00:35:06,719 --> 00:35:09,520
Speaker 1: which have an electric field, and you accelerate them up

696
00:35:09,520 --> 00:35:12,720
Speaker 1: and now you shake them and that wiggles the electric field.

697
00:35:12,960 --> 00:35:15,799
Speaker 1: That wiggle in the electric field is nothing more than

698
00:35:15,920 --> 00:35:20,520
Speaker 1: a photon. It's passing of information and energy through that field.

699
00:35:20,840 --> 00:35:23,160
Speaker 1: So you take a mass, Now it has a curvature

700
00:35:23,160 --> 00:35:26,120
Speaker 1: in space. You wiggle that mass, you accelerate it. That

701
00:35:26,239 --> 00:35:31,720
Speaker 1: wiggling of space time is gravitational radiation. It carries away energy,

702
00:35:32,480 --> 00:35:34,600
Speaker 1: all right. So they're not sort of, you know, aimed

703
00:35:34,600 --> 00:35:37,359
Speaker 1: at each other. They're more like swirling together. But then

704
00:35:37,440 --> 00:35:40,440
Speaker 1: at some point they lose energy and they swirl faster

705
00:35:40,520 --> 00:35:42,600
Speaker 1: and faster and closer and closer, and at some point

706
00:35:42,640 --> 00:35:46,000
Speaker 1: they start to touch, I guess right, or yeah, they

707
00:35:46,000 --> 00:35:47,880
Speaker 1: start to touch. And to think about that, you have

708
00:35:48,000 --> 00:35:52,560
Speaker 1: to think about what you mean by two black holes touching, right, Like,

709
00:35:52,640 --> 00:35:54,560
Speaker 1: what is the edge of a black hole? What's the

710
00:35:54,600 --> 00:35:57,319
Speaker 1: surface of it? Often we talk about it in terms

711
00:35:57,320 --> 00:35:59,800
Speaker 1: of the event horizon. We talked about the event horizon

712
00:35:59,840 --> 00:36:02,319
Speaker 1: as if it's like something physical, you know, like a

713
00:36:02,360 --> 00:36:05,239
Speaker 1: surface or a boundary or something. It's really just sort

714
00:36:05,239 --> 00:36:08,720
Speaker 1: of like a location past which you can never escape

715
00:36:08,719 --> 00:36:11,200
Speaker 1: the black hole. But it's not like there's anything there

716
00:36:11,239 --> 00:36:14,040
Speaker 1: at the event horizon. There's no physical surface. It's just

717
00:36:14,160 --> 00:36:17,279
Speaker 1: like past this point you will never escape. Like the

718
00:36:17,360 --> 00:36:19,279
Speaker 1: edge of a hole is not really a barrier, it's

719
00:36:19,320 --> 00:36:21,200
Speaker 1: just where you fall in. Yeah, it's just where you

720
00:36:21,239 --> 00:36:24,000
Speaker 1: fall in. The subtle point also is that you can't

721
00:36:24,200 --> 00:36:27,399
Speaker 1: measure the event horizon technically. To calculate where the event

722
00:36:27,440 --> 00:36:30,200
Speaker 1: horizon is, you need to know like what happens to

723
00:36:30,239 --> 00:36:32,319
Speaker 1: every particle that comes near it. Then you find sort

724
00:36:32,320 --> 00:36:34,960
Speaker 1: of like the surface in which if a particle passed

725
00:36:34,960 --> 00:36:37,600
Speaker 1: through it, nothing ever escaped, So you sort of need

726
00:36:37,640 --> 00:36:39,719
Speaker 1: to know the fate of every particle to figure out

727
00:36:39,760 --> 00:36:43,400
Speaker 1: exactly where the event horizon is. Wait, wait, what what

728
00:36:43,440 --> 00:36:45,480
Speaker 1: do you mean we can't tell where it is? Like,

729
00:36:45,719 --> 00:36:47,600
Speaker 1: can we do? We just take a picture of a

730
00:36:47,719 --> 00:36:50,040
Speaker 1: black hole recently? Doesn't that give us a pretty good

731
00:36:50,040 --> 00:36:53,239
Speaker 1: idea by the way that the light bends around it

732
00:36:53,640 --> 00:36:56,080
Speaker 1: where the event horizon is. We did take a picture

733
00:36:56,080 --> 00:36:58,840
Speaker 1: of black hole, and that does give us clues about

734
00:36:58,880 --> 00:37:01,360
Speaker 1: the size of the event horizon uson because actually what

735
00:37:01,400 --> 00:37:03,600
Speaker 1: we're seeing there is the shadow of the black hole,

736
00:37:03,960 --> 00:37:06,759
Speaker 1: which is larger than the event horizon because you know,

737
00:37:06,840 --> 00:37:08,719
Speaker 1: some light, for example, will pass near it and get

738
00:37:08,760 --> 00:37:11,080
Speaker 1: bent around it, so the shadow actually looks a little

739
00:37:11,120 --> 00:37:13,480
Speaker 1: bit bigger than the event horizon. But check out our

740
00:37:13,520 --> 00:37:16,399
Speaker 1: whole episode about the black hole image for details about that.

741
00:37:16,560 --> 00:37:19,120
Speaker 1: But in principle, even that picture doesn't tell you exactly

742
00:37:19,160 --> 00:37:21,480
Speaker 1: where the event horizon is. Like it could be that

743
00:37:21,520 --> 00:37:23,720
Speaker 1: there's a particle that could pass a little bit closer

744
00:37:23,760 --> 00:37:25,920
Speaker 1: to the black hole that we're seeing in that picture

745
00:37:25,960 --> 00:37:28,920
Speaker 1: and then escape. You don't know for sure. Now we

746
00:37:29,000 --> 00:37:31,640
Speaker 1: can calculate it, right. General relativity lets you calculate the

747
00:37:31,719 --> 00:37:34,279
Speaker 1: size of the event horizon, so we have this short

748
00:37:34,320 --> 00:37:37,480
Speaker 1: styled radius. But it's not like something you can locally measure.

749
00:37:37,560 --> 00:37:40,000
Speaker 1: You can't say I'm in or I'm out at any

750
00:37:40,040 --> 00:37:42,200
Speaker 1: given moment in the universe. It's not like some device

751
00:37:42,239 --> 00:37:44,840
Speaker 1: you could build that could tell you I'm inside a

752
00:37:44,840 --> 00:37:47,080
Speaker 1: black hole or I'm outside a black hole. You can

753
00:37:47,120 --> 00:37:49,560
Speaker 1: either calculate from general relativity where you can shoot a

754
00:37:49,600 --> 00:37:51,520
Speaker 1: bunch of particles at it and wait till the end

755
00:37:51,520 --> 00:37:53,960
Speaker 1: of the universe and see which one's escaped and which

756
00:37:53,960 --> 00:37:57,040
Speaker 1: ones didn't. So it's sort of a fuzzy boundary, I think,

757
00:37:57,120 --> 00:37:59,200
Speaker 1: is what you're saying exactly, And we're gonna have to

758
00:37:59,280 --> 00:38:01,400
Speaker 1: keep that definitely in mind as we think about what

759
00:38:01,520 --> 00:38:04,080
Speaker 1: happens when the event horizons get close to each other.

760
00:38:04,280 --> 00:38:06,160
Speaker 1: All right, yeah, so what happens? So I have a

761
00:38:06,280 --> 00:38:08,040
Speaker 1: one black hole and I have another black hole and

762
00:38:08,120 --> 00:38:10,120
Speaker 1: meat in my hands, and I'm swirling them and I'm

763
00:38:10,120 --> 00:38:13,120
Speaker 1: bringing them together, and they're swirling and swirling, and at

764
00:38:13,160 --> 00:38:17,239
Speaker 1: some point where the event horizon would be, or where

765
00:38:17,280 --> 00:38:19,359
Speaker 1: we think it is, or fuzzily where it should be,

766
00:38:19,600 --> 00:38:22,120
Speaker 1: they start to overlap, and they start to overlap. And

767
00:38:22,280 --> 00:38:24,320
Speaker 1: when people write to me about this, something they're confused

768
00:38:24,320 --> 00:38:27,920
Speaker 1: about is like a black hole's event horizon is a sphere, right,

769
00:38:27,920 --> 00:38:30,919
Speaker 1: It's like centered around the singularity. Now you have two

770
00:38:30,920 --> 00:38:33,719
Speaker 1: black holes, both of rich or spheres. What happens when

771
00:38:33,760 --> 00:38:37,080
Speaker 1: they touched? You suddenly get a sphere at the center

772
00:38:37,120 --> 00:38:39,080
Speaker 1: of the two? You know, does that mean the event

773
00:38:39,120 --> 00:38:42,279
Speaker 1: horizon is like shrinking a little bit? What happens there?

774
00:38:42,440 --> 00:38:44,840
Speaker 1: And so the answer is you can't have like discontinuities

775
00:38:44,880 --> 00:38:47,040
Speaker 1: with the event horizon is in one place and then

776
00:38:47,280 --> 00:38:51,960
Speaker 1: one instant later it's totally different. It's a smooth transformation

777
00:38:52,200 --> 00:38:55,319
Speaker 1: from happing two blobs to one blob, and a little

778
00:38:55,320 --> 00:38:58,120
Speaker 1: bit surprisingly that means that the event horizon is not

779
00:38:58,360 --> 00:39:02,439
Speaker 1: always spherical. The transition between two black holes and one

780
00:39:02,520 --> 00:39:06,239
Speaker 1: black hole that results it's a weird sort of peanut shape. Yeah,

781
00:39:06,280 --> 00:39:08,400
Speaker 1: I'm imagining. I guess. You know, like if you if

782
00:39:08,400 --> 00:39:11,239
Speaker 1: you take two ink plots, like two blobs of ink

783
00:39:11,400 --> 00:39:13,560
Speaker 1: and you sort of bring them together, they're gonna sort

784
00:39:13,560 --> 00:39:16,640
Speaker 1: of like touch maybe at the boundary and then sort

785
00:39:16,680 --> 00:39:18,960
Speaker 1: of merge and but just a little bit first, and

786
00:39:19,000 --> 00:39:22,120
Speaker 1: then the blobs sort of merges together, the two blobs

787
00:39:22,400 --> 00:39:24,400
Speaker 1: become a peanut shape, and then they sort of blob

788
00:39:24,560 --> 00:39:26,920
Speaker 1: block together. Is that sort of what happens. That's sort

789
00:39:26,920 --> 00:39:29,080
Speaker 1: of what happens. And to figure out exactly what the

790
00:39:29,120 --> 00:39:31,640
Speaker 1: shape of the event horizon is, people do these numerical

791
00:39:31,719 --> 00:39:35,360
Speaker 1: relativity calculations where basically they shoot a bunch of particles

792
00:39:35,480 --> 00:39:37,480
Speaker 1: near these two masses and they figure out where the

793
00:39:37,600 --> 00:39:40,399
Speaker 1: no go zones are, where if a particle passed through

794
00:39:40,440 --> 00:39:42,920
Speaker 1: it it ends up in the singularity no matter what.

795
00:39:43,600 --> 00:39:45,839
Speaker 1: They have to calculate the event horizon in this way

796
00:39:45,880 --> 00:39:48,240
Speaker 1: to like figure out where the no go zones are,

797
00:39:48,600 --> 00:39:50,759
Speaker 1: and they do these incredible simulations and you can find

798
00:39:50,760 --> 00:39:52,920
Speaker 1: these images online if you want. To look at the video.

799
00:39:53,120 --> 00:39:55,040
Speaker 1: We'll put a link into the show notes. And what

800
00:39:55,120 --> 00:39:57,440
Speaker 1: happens is you have like two blobs, and as they

801
00:39:57,440 --> 00:40:00,239
Speaker 1: get closer to each other, there's like a film mint

802
00:40:00,239 --> 00:40:02,640
Speaker 1: that forms between them. Now, the event horizon looks sort

803
00:40:02,640 --> 00:40:04,759
Speaker 1: of like a dumbbells, like two big blocks with a

804
00:40:04,880 --> 00:40:08,000
Speaker 1: very thin line between them. Then as they get closer

805
00:40:08,040 --> 00:40:11,240
Speaker 1: and closer, that line grows and grows and grows. Eventually

806
00:40:11,239 --> 00:40:13,040
Speaker 1: you have like a peanut, and then a tic tac

807
00:40:13,200 --> 00:40:16,480
Speaker 1: and finally a sphere. Wait we skip past the peanut

808
00:40:16,560 --> 00:40:19,360
Speaker 1: m and m or of a whole bunch of other candies.

809
00:40:20,280 --> 00:40:22,960
Speaker 1: All right, well let's get into what actually is happening

810
00:40:22,960 --> 00:40:26,960
Speaker 1: with that event horizon and where do all the gravitational

811
00:40:27,000 --> 00:40:30,520
Speaker 1: waves come from. But first let's take another quick break.

812
00:40:43,400 --> 00:40:46,640
Speaker 1: All right, we're talking about smashing two black holes together.

813
00:40:46,920 --> 00:40:50,680
Speaker 1: And the scenario we're picturing is two black holes that

814
00:40:50,760 --> 00:40:53,000
Speaker 1: came from a set of binary stars and each start

815
00:40:53,080 --> 00:40:55,320
Speaker 1: became a black hole. Now the black holes are swirling

816
00:40:55,360 --> 00:40:57,560
Speaker 1: around each other, getting closer and closer and closer, and

817
00:40:57,880 --> 00:40:59,880
Speaker 1: just as they're about to touch, they actually sort of

818
00:41:00,000 --> 00:41:02,759
Speaker 1: reach out and touch each other kind of in a way. Right, Yeah,

819
00:41:02,760 --> 00:41:06,560
Speaker 1: they become regions in space between the two black holes

820
00:41:06,600 --> 00:41:10,200
Speaker 1: that are now effectively inside their event horizon. They're combined

821
00:41:10,320 --> 00:41:13,680
Speaker 1: event horizon because if you're in that place, you will

822
00:41:13,719 --> 00:41:15,839
Speaker 1: not escape. So you could have been outside the event

823
00:41:15,880 --> 00:41:19,200
Speaker 1: horizon just before, but now this filament has formed where

824
00:41:19,200 --> 00:41:21,880
Speaker 1: if you were right between them, you no longer have

825
00:41:21,920 --> 00:41:24,640
Speaker 1: any chance to escape the black hole. And to me,

826
00:41:24,680 --> 00:41:27,759
Speaker 1: it's really fascinating this moment when the event horizon is

827
00:41:27,880 --> 00:41:31,880
Speaker 1: no longer a sphere, because it's an opportunity to learn something,

828
00:41:31,920 --> 00:41:34,680
Speaker 1: to know something about the history of the black hole.

829
00:41:34,719 --> 00:41:38,480
Speaker 1: What's going on inside even from the outside. What do

830
00:41:38,480 --> 00:41:40,319
Speaker 1: you mean, what what can you learn? What could you

831
00:41:40,360 --> 00:41:42,240
Speaker 1: hope to learn? Well, if you come along a black

832
00:41:42,280 --> 00:41:44,480
Speaker 1: hole and it's a perfect sphere, you have no idea

833
00:41:44,520 --> 00:41:47,600
Speaker 1: what's inside? Is it bananas? Is it apples? Is it

834
00:41:47,680 --> 00:41:50,600
Speaker 1: the result of a star collapsing or two stars collapsing?

835
00:41:50,640 --> 00:41:52,880
Speaker 1: You have no idea about like the merger history of

836
00:41:52,920 --> 00:41:55,080
Speaker 1: that black hole. But if you come along at the

837
00:41:55,120 --> 00:41:57,920
Speaker 1: moment when the black holes are still merging, then you

838
00:41:57,960 --> 00:42:00,719
Speaker 1: know this must have come from too. You know that

839
00:42:00,760 --> 00:42:04,480
Speaker 1: there are two singularities inside that event horizon, or you

840
00:42:04,560 --> 00:42:07,600
Speaker 1: know something about the history of it more so than

841
00:42:07,719 --> 00:42:09,719
Speaker 1: if you just come along to a spear, Right, so

842
00:42:09,760 --> 00:42:12,360
Speaker 1: you know a little bit about what's going on inside

843
00:42:12,360 --> 00:42:15,160
Speaker 1: the event horizon. I see you're saying. It tells you

844
00:42:15,200 --> 00:42:18,080
Speaker 1: a little bit about what happens when you change a

845
00:42:18,080 --> 00:42:21,080
Speaker 1: black hole, right, because a non changing black hole is

846
00:42:21,120 --> 00:42:25,160
Speaker 1: sort of mysterious and impenetrable. But the black holes that's changing,

847
00:42:25,200 --> 00:42:27,640
Speaker 1: maybe you can tell something about whether you know all

848
00:42:27,640 --> 00:42:29,760
Speaker 1: the stuff inside of it is concentrated in the middle

849
00:42:29,920 --> 00:42:32,560
Speaker 1: or spread out evenly, things like that. Yeah, it's fascinating

850
00:42:32,560 --> 00:42:34,960
Speaker 1: to me because black holes are like the most identical

851
00:42:35,040 --> 00:42:37,959
Speaker 1: thing in the universe. Remember this, in theory, only three

852
00:42:38,000 --> 00:42:40,440
Speaker 1: things to know about a black hole the only three

853
00:42:40,520 --> 00:42:43,400
Speaker 1: numbers that totally determine it, and two black holes that

854
00:42:43,440 --> 00:42:46,960
Speaker 1: have the same mass, spin, and charge are totally equivalent.

855
00:42:46,960 --> 00:42:49,239
Speaker 1: There's no way you can do experiments to tell them

856
00:42:49,239 --> 00:42:52,759
Speaker 1: apart except unless and this is the crack in the

857
00:42:52,800 --> 00:42:55,000
Speaker 1: no hair theorem. If you have a black hole with

858
00:42:55,120 --> 00:42:57,960
Speaker 1: that mass and that's been that charge, but it's still

859
00:42:58,000 --> 00:43:01,120
Speaker 1: finishing its last merger, you can know one little clue

860
00:43:01,160 --> 00:43:03,239
Speaker 1: about that black hole. You can know that it came

861
00:43:03,320 --> 00:43:05,640
Speaker 1: from this merger, and that must mean that the inners

862
00:43:05,640 --> 00:43:08,480
Speaker 1: of the black hole haven't quite settled down yet. They

863
00:43:08,520 --> 00:43:11,200
Speaker 1: haven't like formed the singularity or the quantum fuzz of

864
00:43:11,200 --> 00:43:14,080
Speaker 1: all or whatever is going on inside. Because the event

865
00:43:14,080 --> 00:43:17,359
Speaker 1: horizon has a different shape. It's the same mass, the

866
00:43:17,400 --> 00:43:20,000
Speaker 1: same spin, and the same charge, but a different shape.

867
00:43:20,000 --> 00:43:22,960
Speaker 1: Event horizon hasn't yet collapsed into a sphere. Oh. I

868
00:43:23,000 --> 00:43:26,760
Speaker 1: see you're saying, we can learn about the resulting black holes,

869
00:43:26,800 --> 00:43:29,480
Speaker 1: but we don't really wouldn't know anything about the holes.

870
00:43:29,600 --> 00:43:32,520
Speaker 1: The two holes that went into it right like they would,

871
00:43:32,520 --> 00:43:34,320
Speaker 1: Those would still be a mystery. Those would be a

872
00:43:34,360 --> 00:43:36,080
Speaker 1: little bit of a mystery. But you can know something

873
00:43:36,120 --> 00:43:39,239
Speaker 1: about their relative masses. For example, if two black holes

874
00:43:39,280 --> 00:43:41,880
Speaker 1: that are equal in mass merge, then as they're merging,

875
00:43:42,080 --> 00:43:44,440
Speaker 1: they look different than a black hole where one was

876
00:43:44,480 --> 00:43:47,160
Speaker 1: like of the final mass and the other one was

877
00:43:47,200 --> 00:43:50,640
Speaker 1: one because it's more asymmetric. So you know something about

878
00:43:50,640 --> 00:43:52,759
Speaker 1: what went into the black hole from the shape of

879
00:43:52,760 --> 00:43:55,960
Speaker 1: the sort of peanut before it collapses into a sphere.

880
00:43:56,320 --> 00:43:58,960
Speaker 1: I just think that's fascinating because it's a tiny little crack,

881
00:43:59,200 --> 00:44:01,880
Speaker 1: and any crack to say, like, I know something about

882
00:44:01,880 --> 00:44:05,480
Speaker 1: what's going on past the event horizon. That's tantalizing because

883
00:44:05,480 --> 00:44:07,880
Speaker 1: I mean, it was so little about what's inside. I

884
00:44:07,920 --> 00:44:10,160
Speaker 1: see you're saying, like a regular black hole by itself,

885
00:44:10,200 --> 00:44:12,759
Speaker 1: it's inscrutable. But if you see what two of them

886
00:44:12,800 --> 00:44:14,920
Speaker 1: joining together, you're like, hey, I know a little bit

887
00:44:14,960 --> 00:44:18,279
Speaker 1: about what happens in these extreme conditions. Yeah, you know

888
00:44:18,320 --> 00:44:20,319
Speaker 1: a little bit about the history of this black hole,

889
00:44:20,360 --> 00:44:23,160
Speaker 1: whereas for an other normal black hole, you know literally

890
00:44:23,320 --> 00:44:26,560
Speaker 1: zilch except for the mass, spin and the charge. And

891
00:44:26,600 --> 00:44:29,200
Speaker 1: here you have like a little bit more information. Plus

892
00:44:29,239 --> 00:44:31,239
Speaker 1: you get to describe these things in terms of a

893
00:44:31,280 --> 00:44:34,799
Speaker 1: diagram the physicists called a pair of pants diagram, which

894
00:44:34,840 --> 00:44:37,480
Speaker 1: is a lot of fun. Yeah. I guess if you

895
00:44:37,520 --> 00:44:40,919
Speaker 1: google pants and black holes, you'll get a whole bunch

896
00:44:40,960 --> 00:44:45,520
Speaker 1: of interesting images. I haven't tried it to make we

897
00:44:45,640 --> 00:44:49,399
Speaker 1: should maybe should have. The adults in the audience checked

898
00:44:49,440 --> 00:44:51,680
Speaker 1: that first. The ideas that you have two patches of

899
00:44:51,719 --> 00:44:53,799
Speaker 1: space time, which is sort of like the legs of

900
00:44:53,840 --> 00:44:56,440
Speaker 1: the pants, and then they're merging and they form like

901
00:44:56,520 --> 00:44:59,480
Speaker 1: the waist eventually. So if you draw that out with

902
00:44:59,520 --> 00:45:02,359
Speaker 1: like two of space time connecting each other, you start

903
00:45:02,360 --> 00:45:04,120
Speaker 1: with two, you end with one. It's sort of like

904
00:45:04,160 --> 00:45:07,080
Speaker 1: a pair of pants. Yeah, I think it's very hard

905
00:45:07,120 --> 00:45:08,760
Speaker 1: to paint that picture. But I think the main point

906
00:45:08,800 --> 00:45:11,200
Speaker 1: is that when the two black holes get together, they

907
00:45:11,239 --> 00:45:13,840
Speaker 1: sort of reach out in the middle, they start merging

908
00:45:13,840 --> 00:45:15,799
Speaker 1: that sort of I guess whether you're in scene would

909
00:45:15,800 --> 00:45:18,640
Speaker 1: be in the pants. And then they blocked together, right,

910
00:45:19,080 --> 00:45:20,799
Speaker 1: Is that sort of what happens? Like? Is that what this?

911
00:45:20,920 --> 00:45:22,920
Speaker 1: At least that's what the simulations say, that they just

912
00:45:23,600 --> 00:45:26,600
Speaker 1: blocked together and become one big hole. Yeah, they blocked

913
00:45:26,600 --> 00:45:29,160
Speaker 1: together and become one big hole and in the process

914
00:45:29,160 --> 00:45:32,480
Speaker 1: released an incredible amount of gravitational radiation. And we can

915
00:45:32,560 --> 00:45:35,600
Speaker 1: learn something about that process from looking at the details

916
00:45:35,640 --> 00:45:38,640
Speaker 1: of the wiggles of that radiation, right, And a lot

917
00:45:38,680 --> 00:45:42,359
Speaker 1: of this energy comes from the angular momentum, right, Like

918
00:45:42,560 --> 00:45:46,320
Speaker 1: maybe they're spinning around each other slowly when they're far apart,

919
00:45:46,400 --> 00:45:48,560
Speaker 1: But then when as the two black holes get together,

920
00:45:48,680 --> 00:45:51,239
Speaker 1: they have to preserve the same angular momentum as other.

921
00:45:51,520 --> 00:45:53,359
Speaker 1: By the time they get really really close each other,

922
00:45:53,400 --> 00:45:57,879
Speaker 1: they're spinning at incredible speeds, right, which makes for huge accelerations,

923
00:45:57,880 --> 00:46:00,759
Speaker 1: which make for a huge gravitational way. And that's why

924
00:46:00,800 --> 00:46:04,600
Speaker 1: probably every black hole out there is spinning the simplest

925
00:46:04,680 --> 00:46:06,640
Speaker 1: idea we have of a black hole, the short stile

926
00:46:06,719 --> 00:46:09,640
Speaker 1: black hole of a sphere is in the event that

927
00:46:09,680 --> 00:46:11,880
Speaker 1: the mass is not spinning, is just sitting there. But

928
00:46:12,040 --> 00:46:14,399
Speaker 1: because things fall into a black hole, and they will

929
00:46:14,440 --> 00:46:17,960
Speaker 1: always swirl around before they fall in, because otherwise they

930
00:46:18,040 --> 00:46:20,400
Speaker 1: have to fall in directly to the center of like

931
00:46:20,680 --> 00:46:24,839
Speaker 1: perfectly online with the singularity. Any deviation from that, they're

932
00:46:24,840 --> 00:46:27,080
Speaker 1: gonna fall in with a little bit of angular velocity

933
00:46:27,280 --> 00:46:30,040
Speaker 1: and so with momentum, and so they're gonna end up spinning.

934
00:46:30,040 --> 00:46:32,480
Speaker 1: So the final black hole has to be spinning. Every

935
00:46:32,520 --> 00:46:35,600
Speaker 1: black hole out there in the universe is almost certainly

936
00:46:35,680 --> 00:46:39,120
Speaker 1: spinning for that reason. And two black hole spinning around

937
00:46:39,200 --> 00:46:42,080
Speaker 1: each other, you're absolutely right, how a lot of angular momentum,

938
00:46:42,280 --> 00:46:44,680
Speaker 1: and they're going to generate a lot of gravitational radiation.

939
00:46:44,920 --> 00:46:48,000
Speaker 1: But the end result, what ends up happening at the

940
00:46:48,080 --> 00:46:50,480
Speaker 1: end is the emerge into one bigger black hole that's

941
00:46:50,520 --> 00:46:53,960
Speaker 1: bigger than the two individual black holes, but maybe like

942
00:46:54,120 --> 00:46:56,600
Speaker 1: not as big as if you just added the mass

943
00:46:56,600 --> 00:46:59,400
Speaker 1: of the two black holes exactly. They lose some of

944
00:46:59,440 --> 00:47:02,560
Speaker 1: that map ass, right, what happens when you lose energy

945
00:47:02,640 --> 00:47:05,520
Speaker 1: as a black hole, you lose mass, just like if

946
00:47:05,560 --> 00:47:09,440
Speaker 1: a black hole is radiating Hawking radiation, it's shooting out particles,

947
00:47:09,480 --> 00:47:12,719
Speaker 1: it's losing mass, and so if therefore it's shrinking, right,

948
00:47:12,719 --> 00:47:15,640
Speaker 1: So black holes can evaporate. They can lose their mass

949
00:47:15,640 --> 00:47:18,560
Speaker 1: through hawking radiation and get smaller and smaller. If they

950
00:47:18,600 --> 00:47:23,600
Speaker 1: also lose energy by gravitational radiation, they are also getting smaller.

951
00:47:24,000 --> 00:47:27,839
Speaker 1: And so there's so much energy released in these collisions

952
00:47:27,880 --> 00:47:30,120
Speaker 1: that sometimes they can lose a lot of mass, like

953
00:47:30,239 --> 00:47:33,440
Speaker 1: as much mass is our sun, right, and this energy

954
00:47:33,520 --> 00:47:36,440
Speaker 1: goes out as gravitational ways. But also I imagine a

955
00:47:36,480 --> 00:47:39,440
Speaker 1: whole bunch of like light to write like quasars have

956
00:47:40,120 --> 00:47:42,319
Speaker 1: you know, all that gas that was around each of

957
00:47:42,320 --> 00:47:46,080
Speaker 1: them is you know, going through these extreme velocities and

958
00:47:46,360 --> 00:47:48,319
Speaker 1: smashing against each other. A lot of that must go

959
00:47:48,360 --> 00:47:51,240
Speaker 1: out as basically light as well. Most of the energy

960
00:47:51,320 --> 00:47:54,880
Speaker 1: is radiated as gravitational radiation. It can be like five

961
00:47:55,840 --> 00:47:58,400
Speaker 1: of the mass of the system is lost due to

962
00:47:58,440 --> 00:48:01,800
Speaker 1: gravitational radiation. Can also be light emitted, and this is

963
00:48:01,840 --> 00:48:04,080
Speaker 1: sort of an open question. People have only seen a

964
00:48:04,120 --> 00:48:07,520
Speaker 1: couple examples where they have seen flashes of light perfectly

965
00:48:07,560 --> 00:48:11,120
Speaker 1: coincident with black hole collisions, and so something they're excited

966
00:48:11,160 --> 00:48:14,080
Speaker 1: to study. This is an era of multi messenger astronomy

967
00:48:14,080 --> 00:48:16,680
Speaker 1: when you can see the same thing you know, electromagnetic

968
00:48:16,760 --> 00:48:19,680
Speaker 1: radiation light as you can in gravitational radiation, and so

969
00:48:19,760 --> 00:48:22,520
Speaker 1: you can study it much more deeply. It's not something

970
00:48:22,560 --> 00:48:24,960
Speaker 1: we've seen many examples of, so it's not something that's

971
00:48:25,040 --> 00:48:27,520
Speaker 1: very well understood yet. All right, so stay tuned as

972
00:48:27,520 --> 00:48:30,440
Speaker 1: we get more samples of these collisions. But I guess, well,

973
00:48:30,480 --> 00:48:32,360
Speaker 1: one big question. It kind of goes back to what

974
00:48:32,360 --> 00:48:34,960
Speaker 1: you were saying before, which is that you know, time

975
00:48:35,280 --> 00:48:37,560
Speaker 1: slows down near a black hole. So if you're if

976
00:48:37,560 --> 00:48:41,120
Speaker 1: I'm near a black hole, my time is frozen basically

977
00:48:41,280 --> 00:48:43,879
Speaker 1: or it's super slow motion. So how do these But

978
00:48:43,880 --> 00:48:46,000
Speaker 1: but now, if you get a black hole nextly the

979
00:48:46,040 --> 00:48:48,920
Speaker 1: other one, isn't one of them slowing time down for

980
00:48:49,000 --> 00:48:51,480
Speaker 1: the other one? And wouldn't they just look to us

981
00:48:51,520 --> 00:48:53,960
Speaker 1: like they're frozen in time? Yeah, you might wonder, like

982
00:48:54,080 --> 00:48:56,680
Speaker 1: why do black holes ever collide? Don't they slow each

983
00:48:56,719 --> 00:48:59,839
Speaker 1: other's time down so much that they basically just get

984
00:49:00,080 --> 00:49:03,279
Speaker 1: rozen before they merge? Right, Remember that a black hole

985
00:49:03,440 --> 00:49:06,719
Speaker 1: is not a single point in space, So really, what

986
00:49:06,760 --> 00:49:10,160
Speaker 1: we're talking about is the merger of their event horizons.

987
00:49:10,280 --> 00:49:13,560
Speaker 1: And so while the two singularities may orbit each other

988
00:49:13,600 --> 00:49:16,600
Speaker 1: for a long time, slowing down because of the time dilation,

989
00:49:16,840 --> 00:49:21,680
Speaker 1: their event horizons can merge before the singularities come together. Right,

990
00:49:21,680 --> 00:49:25,560
Speaker 1: but still, like the time should be slowing down almost

991
00:49:25,600 --> 00:49:28,080
Speaker 1: to a stand still near the edge of each black hole,

992
00:49:28,640 --> 00:49:32,319
Speaker 1: so as they start to merge, when things kind of

993
00:49:32,360 --> 00:49:35,600
Speaker 1: freezing time. So things sort of do freezing time in

994
00:49:35,640 --> 00:49:38,120
Speaker 1: the sense that they get slowed down. Like what are

995
00:49:38,120 --> 00:49:40,680
Speaker 1: we seeing when we see black holes merge? We see

996
00:49:40,680 --> 00:49:44,279
Speaker 1: a pattern of gravitational radiation that comes from the black hole.

997
00:49:44,640 --> 00:49:46,560
Speaker 1: We see its speed up and go faster and faster

998
00:49:46,640 --> 00:49:49,279
Speaker 1: and faster. Now, when you look at that, you might wonder, like,

999
00:49:49,520 --> 00:49:51,920
Speaker 1: why isn't that slowed down? Why isn't it get like

1000
00:49:52,200 --> 00:49:54,239
Speaker 1: spread out and slowed down. Why don't we see the

1001
00:49:54,239 --> 00:49:57,160
Speaker 1: gravitational radiation gets slower and slower. The answer is that

1002
00:49:57,200 --> 00:49:59,759
Speaker 1: we are. We are seeing the effects of that time

1003
00:49:59,800 --> 00:50:03,359
Speaker 1: down lation already. Like if there wasn't time dilation, then

1004
00:50:03,360 --> 00:50:06,239
Speaker 1: that gravitational radiation just for the collision would be going

1005
00:50:06,280 --> 00:50:09,799
Speaker 1: insanely fast. So we are seeing the effects of time

1006
00:50:09,840 --> 00:50:12,520
Speaker 1: dilation already. Sort of build in. When we see black

1007
00:50:12,560 --> 00:50:16,080
Speaker 1: holes collide, it would look different without the time dilation. Oh,

1008
00:50:16,280 --> 00:50:19,239
Speaker 1: I see, you're saying, like things are so extreme. Things

1009
00:50:19,280 --> 00:50:24,200
Speaker 1: are moving so fast around these collisions, and gravitational ways

1010
00:50:24,239 --> 00:50:28,360
Speaker 1: are being emitted so quickly and so intensely that even

1011
00:50:28,440 --> 00:50:31,920
Speaker 1: with almost freezing time, they still come out and they

1012
00:50:31,920 --> 00:50:35,200
Speaker 1: seem at a sort of a certain frequency for us exactly.

1013
00:50:35,440 --> 00:50:38,120
Speaker 1: That's built into those calculations, and we do the numerical

1014
00:50:38,160 --> 00:50:40,440
Speaker 1: relativity to figure out like what's happening, and where is

1015
00:50:40,440 --> 00:50:43,799
Speaker 1: the event horizon, how much gravitational radiation is emitted. That's

1016
00:50:43,840 --> 00:50:46,680
Speaker 1: of course taken into account, and so we're seeing just

1017
00:50:46,719 --> 00:50:50,840
Speaker 1: what we expect time dilated, slowed down collision, but still

1018
00:50:50,880 --> 00:50:54,800
Speaker 1: generating these gravitational waves, so it's not slowed down to zero.

1019
00:50:55,239 --> 00:50:56,920
Speaker 1: I see. So if you are like near one of

1020
00:50:56,960 --> 00:50:59,719
Speaker 1: these black holes as an observer, like it would be

1021
00:50:59,760 --> 00:51:03,080
Speaker 1: like insane, right, It wouild just like happen in a flash. Yes, exactly,

1022
00:51:03,080 --> 00:51:05,319
Speaker 1: would happened much more quickly. If you were very close

1023
00:51:05,360 --> 00:51:07,920
Speaker 1: to the event horizons of these black holes as they

1024
00:51:07,920 --> 00:51:10,000
Speaker 1: were happening, so you had sort of the same clock

1025
00:51:10,120 --> 00:51:12,759
Speaker 1: as they would, you would see something very different. Just

1026
00:51:12,800 --> 00:51:14,440
Speaker 1: the same way if you see somebody fall into a

1027
00:51:14,480 --> 00:51:17,040
Speaker 1: black hole from far away, you see their time getting

1028
00:51:17,040 --> 00:51:20,080
Speaker 1: slowed down, but they don't see that, right, they experienced

1029
00:51:20,120 --> 00:51:22,200
Speaker 1: time normally. They just fall in and end up hitting

1030
00:51:22,239 --> 00:51:24,480
Speaker 1: the singularity if you look very very different, if you

1031
00:51:24,520 --> 00:51:26,880
Speaker 1: were in the neighborhood of the black hole. Mm. So

1032
00:51:26,960 --> 00:51:29,359
Speaker 1: that's pretty convenient, right, Like, usually when you want to

1033
00:51:29,440 --> 00:51:32,200
Speaker 1: observe something colliding really fast, you have to use a

1034
00:51:32,239 --> 00:51:34,920
Speaker 1: high speed camera or you have to somehow slow down

1035
00:51:35,160 --> 00:51:38,040
Speaker 1: time or sampled super fast that you get a good

1036
00:51:38,040 --> 00:51:39,600
Speaker 1: picture of what's going up. This one has sort of

1037
00:51:39,640 --> 00:51:43,960
Speaker 1: like a built in slow mo setting. Exactly when the

1038
00:51:43,960 --> 00:51:46,800
Speaker 1: most interesting thing happens in the universe, it automatically goes slow,

1039
00:51:47,160 --> 00:51:49,839
Speaker 1: just like in special effects in the movies, right, just

1040
00:51:49,880 --> 00:51:52,800
Speaker 1: like in Marvel movies, where like the bad guy shoots

1041
00:51:52,800 --> 00:51:55,160
Speaker 1: at the good guy and it's like time slows down

1042
00:51:56,560 --> 00:51:59,000
Speaker 1: so they can dodge it. Yeah, exactly, just like in

1043
00:51:59,040 --> 00:52:01,880
Speaker 1: the matrix they can make those crazy bends and dodge

1044
00:52:01,920 --> 00:52:04,560
Speaker 1: those bullets. All right, Well, I guess then that's what

1045
00:52:04,880 --> 00:52:07,279
Speaker 1: happens when you collide to black holes. They sort of

1046
00:52:07,400 --> 00:52:10,200
Speaker 1: slowly reach out to each other. They start to merge,

1047
00:52:10,200 --> 00:52:13,279
Speaker 1: you get a peanut shaped black hole, I guess, and

1048
00:52:13,320 --> 00:52:16,360
Speaker 1: then that eventually blogs into a bigger black hole. And

1049
00:52:16,440 --> 00:52:19,840
Speaker 1: some folks write and ask questions like, is it possible

1050
00:52:19,880 --> 00:52:22,880
Speaker 1: for particles to escape the black hole during the merger

1051
00:52:23,160 --> 00:52:25,279
Speaker 1: because they've heard the black holes shrink a little bit

1052
00:52:25,320 --> 00:52:29,000
Speaker 1: they radiate this energy away, and so like, maybe when

1053
00:52:29,040 --> 00:52:31,919
Speaker 1: the black holes are combining, something can like sneak out

1054
00:52:31,960 --> 00:52:35,200
Speaker 1: the back, right, which is a fun idea, But unfortunately no,

1055
00:52:35,680 --> 00:52:38,600
Speaker 1: black holes do not leak out any of this information

1056
00:52:38,719 --> 00:52:41,120
Speaker 1: when they emerge. And the key thing to understand is

1057
00:52:41,160 --> 00:52:43,680
Speaker 1: that even though the mass of the two black holes

1058
00:52:43,760 --> 00:52:46,800
Speaker 1: is smaller than there's some the volume of a black

1059
00:52:46,800 --> 00:52:50,000
Speaker 1: hole grows very quickly with its mass. So even though

1060
00:52:50,040 --> 00:52:51,840
Speaker 1: the final mass is not just the sum of the

1061
00:52:51,840 --> 00:52:55,240
Speaker 1: incoming mass, the final volume can be like eight times

1062
00:52:55,280 --> 00:52:58,560
Speaker 1: the original black hole volume. So the event horizon is

1063
00:52:58,760 --> 00:53:01,520
Speaker 1: smaller than it would have been if it hadn't radiated

1064
00:53:01,520 --> 00:53:04,759
Speaker 1: gravitational radiation, but it's still bigger than either of the

1065
00:53:04,800 --> 00:53:09,239
Speaker 1: two black holes combined. But you're saying, I think some

1066
00:53:09,320 --> 00:53:13,160
Speaker 1: things do sort of escape, right, Some information escapes, right,

1067
00:53:13,480 --> 00:53:15,920
Speaker 1: like even if it's in a different form in the

1068
00:53:15,960 --> 00:53:19,120
Speaker 1: form of gravitational waves. I think you're saying earlier that

1069
00:53:19,239 --> 00:53:21,040
Speaker 1: you know, you can learn a little bit of the

1070
00:53:21,200 --> 00:53:24,839
Speaker 1: its history as stuff escapes, right, that's information, right, Yeah,

1071
00:53:24,840 --> 00:53:27,560
Speaker 1: the gravitational waves contain information about the mass of the

1072
00:53:27,600 --> 00:53:30,960
Speaker 1: black hole and its location and its velocity. Doesn't tell

1073
00:53:30,960 --> 00:53:33,680
Speaker 1: you anything about what's going on inside. But you're right,

1074
00:53:33,719 --> 00:53:35,680
Speaker 1: from the shape of the event horizon, you can tell

1075
00:53:35,719 --> 00:53:38,800
Speaker 1: a little bit about the history of this black hole.

1076
00:53:39,080 --> 00:53:42,080
Speaker 1: And you're right, that's also encoded in the gravitational waves.

1077
00:53:42,080 --> 00:53:43,960
Speaker 1: But if something was just like at the edge of

1078
00:53:43,960 --> 00:53:47,080
Speaker 1: the black hole as it was merging, could somehow, you know,

1079
00:53:48,080 --> 00:53:50,800
Speaker 1: get lucky and somehow, you know, as these things are merging,

1080
00:53:50,840 --> 00:53:53,719
Speaker 1: it maybe pools on the event horizon in such a

1081
00:53:53,719 --> 00:53:55,440
Speaker 1: way that somehow it gives you a little bit of

1082
00:53:55,480 --> 00:53:59,000
Speaker 1: a window for like one particle to like shoot out. No,

1083
00:53:59,320 --> 00:54:02,640
Speaker 1: unfortunately not, that's what the event horizon means. The event

1084
00:54:02,640 --> 00:54:04,960
Speaker 1: horizon is not a physical surface, is just like the

1085
00:54:05,000 --> 00:54:09,279
Speaker 1: location past which no information ever actually gets out, so

1086
00:54:09,320 --> 00:54:11,239
Speaker 1: you can't ask, like, is it possible for something to

1087
00:54:11,239 --> 00:54:13,719
Speaker 1: get out? Well, that's like by definition, that's what the

1088
00:54:13,719 --> 00:54:16,680
Speaker 1: event horizon is. It's the point where nothing ever escapes,

1089
00:54:16,920 --> 00:54:19,640
Speaker 1: no information leaks out. That's how we figure out where

1090
00:54:19,640 --> 00:54:22,680
Speaker 1: the event horizon is for these things at any given moment.

1091
00:54:23,000 --> 00:54:25,360
Speaker 1: We look into the future history of these black holes

1092
00:54:25,360 --> 00:54:28,040
Speaker 1: in our simulation and say, where's the point pass which

1093
00:54:28,160 --> 00:54:31,239
Speaker 1: nothing ever escapes? Right right? I guess I'm thinking, like,

1094
00:54:31,320 --> 00:54:34,320
Speaker 1: you know, like, if you're accelerating the black hole really fast,

1095
00:54:34,719 --> 00:54:37,120
Speaker 1: isn't it possible for something to escape? You know, like

1096
00:54:37,600 --> 00:54:40,640
Speaker 1: if I accelerated the Earth really fast, the things on

1097
00:54:40,640 --> 00:54:42,799
Speaker 1: one side would be squished against the Earth, but maybe

1098
00:54:42,840 --> 00:54:45,120
Speaker 1: the things on the other side of the Earth might

1099
00:54:45,200 --> 00:54:48,080
Speaker 1: fly off and get left behind. It's certainly true that

1100
00:54:48,120 --> 00:54:50,200
Speaker 1: if you did that to the Earth you would cause

1101
00:54:50,360 --> 00:54:53,000
Speaker 1: incredible damage. And I like the way you're thinking about

1102
00:54:53,040 --> 00:54:55,799
Speaker 1: really destructive experiments just to learn about the nature of

1103
00:54:55,840 --> 00:54:59,239
Speaker 1: the universe. Kudos they're you're the becoming a physicist. But

1104
00:54:59,280 --> 00:55:01,200
Speaker 1: if you did that to black hole, you with nothing

1105
00:55:01,200 --> 00:55:03,640
Speaker 1: would leak out of the event horizon. That black hole

1106
00:55:03,680 --> 00:55:06,200
Speaker 1: is enough curvature that even photons moving at the speed

1107
00:55:06,239 --> 00:55:08,640
Speaker 1: of light can't escape, and by accelerating the black hole

1108
00:55:08,719 --> 00:55:11,239
Speaker 1: can't make anything travel faster than the speed of one.

1109
00:55:11,360 --> 00:55:14,719
Speaker 1: All right, it seems like it's plausible well, but I

1110
00:55:14,719 --> 00:55:17,520
Speaker 1: think the main question is what happens when two black

1111
00:55:17,520 --> 00:55:20,000
Speaker 1: holes collide, And they sort of don't collide, right, they

1112
00:55:20,000 --> 00:55:23,000
Speaker 1: sort of smushed together. I guess it's the simple answer.

1113
00:55:23,480 --> 00:55:25,640
Speaker 1: They sort of grow to meet each other and for

1114
00:55:25,680 --> 00:55:27,960
Speaker 1: a few moments there you have a black hole that

1115
00:55:28,040 --> 00:55:31,440
Speaker 1: doesn't have a spherical event horizon, which is kind of

1116
00:55:31,480 --> 00:55:35,200
Speaker 1: an incredible revealing moment for the black hole. Yeah, you

1117
00:55:35,239 --> 00:55:39,399
Speaker 1: get a peanut, I guess, peanut black hole. All right, Well,

1118
00:55:39,440 --> 00:55:41,600
Speaker 1: I think this really kind of points to some of

1119
00:55:41,600 --> 00:55:44,200
Speaker 1: the amazing things that can happen out there in the universe.

1120
00:55:44,280 --> 00:55:48,080
Speaker 1: You know, the situations with that are not just extreme,

1121
00:55:48,160 --> 00:55:50,360
Speaker 1: but it's like you take two extreme situations and you

1122
00:55:50,400 --> 00:55:53,719
Speaker 1: smash them together, you get like extra extreme. The thing

1123
00:55:53,760 --> 00:55:56,439
Speaker 1: that amazes me is that we can do these calculations.

1124
00:55:56,440 --> 00:56:00,560
Speaker 1: People perform these simulations using numerical relativity tools. They described

1125
00:56:00,600 --> 00:56:03,640
Speaker 1: these incredible bonkers things that's happening, and then we can

1126
00:56:03,680 --> 00:56:06,080
Speaker 1: actually look out there in the universe and we see them.

1127
00:56:06,120 --> 00:56:09,120
Speaker 1: It really happens, and it makes you wonder, like, is

1128
00:56:09,160 --> 00:56:11,040
Speaker 1: this what's really going on out there? If I could

1129
00:56:11,120 --> 00:56:13,520
Speaker 1: fly out to the black hole and like watch it

1130
00:56:13,560 --> 00:56:16,239
Speaker 1: with my eyeballs. Is this what I would see? You know?

1131
00:56:16,320 --> 00:56:18,520
Speaker 1: And I hope that one day, eventually we can't travel

1132
00:56:18,520 --> 00:56:20,359
Speaker 1: the universe and we don't have to just see these

1133
00:56:20,360 --> 00:56:23,200
Speaker 1: black holes from billions of light years away. We could

1134
00:56:23,200 --> 00:56:25,759
Speaker 1: see these collisions close up. Yeah, just make sure you

1135
00:56:25,800 --> 00:56:29,279
Speaker 1: bring some peanuts to snack on while you watch, and

1136
00:56:29,320 --> 00:56:31,760
Speaker 1: smash your peanuts together with a chocolate bar and boom,

1137
00:56:31,800 --> 00:56:37,000
Speaker 1: you invented chocolate. Eminem's that's too extreme, Daniel extreme snacking

1138
00:56:37,040 --> 00:56:39,680
Speaker 1: with Daniel and Jorge. All right, well, we hope you

1139
00:56:39,760 --> 00:56:42,360
Speaker 1: enjoyed that. And think about all the amazing things that

1140
00:56:42,400 --> 00:56:44,799
Speaker 1: are happening right now in the universe. Who's you know

1141
00:56:44,960 --> 00:56:47,920
Speaker 1: echoes we're hearing right now that are washing through right

1142
00:56:47,920 --> 00:56:51,360
Speaker 1: now and maybe telling you about what happened in that collision.

1143
00:56:51,600 --> 00:56:53,080
Speaker 1: Think about all the things that are happening in the

1144
00:56:53,160 --> 00:56:55,680
Speaker 1: universe and sending us information that we don't even know

1145
00:56:55,719 --> 00:56:59,759
Speaker 1: about that we're ignoring that future generations of scientists will

1146
00:56:59,760 --> 00:57:02,920
Speaker 1: just cover and we'll use to learn incredible things about

1147
00:57:02,920 --> 00:57:05,680
Speaker 1: the universe. Yeah. I mean, there must have been hundreds

1148
00:57:05,760 --> 00:57:08,960
Speaker 1: or thousands or hundreds of thousands of black hole collisions.

1149
00:57:09,239 --> 00:57:13,880
Speaker 1: Who's crash, whose mush sounds washed over humanity, but we

1150
00:57:13,960 --> 00:57:16,960
Speaker 1: never even knew. We see a tiny, tiny fraction of

1151
00:57:17,000 --> 00:57:20,600
Speaker 1: the universe, and we understand even lesson. Thanks for joining us,

1152
00:57:21,280 --> 00:57:31,280
Speaker 1: see you next time. Thanks for listening, and remember that

1153
00:57:31,400 --> 00:57:34,200
Speaker 1: Daniel and Jorge explain the Universe is a production of

1154
00:57:34,280 --> 00:57:37,640
Speaker 1: I Heart Radio. Or more podcast from my heart Radio,

1155
00:57:37,760 --> 00:57:41,360
Speaker 1: visit the I heart Radio app, Apple Podcasts, or wherever

1156
00:57:41,480 --> 00:57:43,160
Speaker 1: you listen to your favorite shows.