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Speaker 1: Hey, or Hey. You know how sometimes everybody thinks they

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Speaker 1: know the answer to a question, but they're actually all wrong.

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Speaker 1: You mean, like how you think everything weird in space

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Speaker 1: is because of aliens. Well, that's not a good example.

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Speaker 1: I think it probably is because of aliens. Or you mean, like,

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Speaker 1: what why people think this guy is blue? Yeah, a

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Speaker 1: lot of people think this guy is blue because of

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Speaker 1: the ocean. Wait, it's not because of the ocean. Do

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Speaker 1: you even listen to our podcast? We did a whole

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Speaker 1: episode about that. I don't listen to our podcast. I'm

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Speaker 1: too busy looking out for aliens. Well, if you did

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Speaker 1: pay attention, sometimes you'd realize that sometimes there's a question

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Speaker 1: in science that everybody assumes they know the answer to,

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Speaker 1: but it turns out they don't. Hi. I'm or Hey.

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Speaker 1: I'm a cartoonists and the creator of PhD comics. Hi

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Speaker 1: I'm Daniel. I'm a podcast host and part time particle physicist.

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Speaker 1: Have you been downgraded to part time? Now? I decided

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Speaker 1: let's make this podcast thing my primary activity. That's right,

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Speaker 1: it's two hours a week, but it's the most important

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Speaker 1: and valuable two hours of my week. Two hours of work.

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Speaker 1: Isn't that too much? For a physicist. Well, you know,

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Speaker 1: you've got your naps in, you've got your coffee breaks,

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Speaker 1: you got your scribbling nonsense on the board to look busy.

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Speaker 1: So it's a pretty full day after a while, you

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Speaker 1: mean a pretty full week, pretty for a week. Yeah,

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Speaker 1: you know. But I modeled my work day after my

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Speaker 1: um my cartooning role models. You know. Yeah, sleep in,

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Speaker 1: never change out of your pajamas, this kind of stuff. Yeah, No,

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Speaker 1: we should all look up to cartoonists as a nation.

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Speaker 1: We would all be more productive if we follow the

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Speaker 1: cartooning work week. We'd all be a lot more funny,

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Speaker 1: that's right. We would do the low way to prosperity.

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Speaker 1: But you are listeners are listening to our podcast, Daniel

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Speaker 1: and Jorge Explain the Universe, a production of I Heart Radio,

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Speaker 1: in which we take weird and funny and amazing and

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Speaker 1: crazy things about the universe and try to doodle them

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Speaker 1: into your brain with silly analogies and bad jokes. That's right.

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Speaker 1: We try to take you to the corners, the far

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Speaker 1: reaching corners of the universe, and to explore the heaviest things,

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Speaker 1: the biggest things, the brightest things, the smallest things that

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Speaker 1: are out there for us to discover that's right, And

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Speaker 1: so we have this series of podcasts we've been really

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Speaker 1: enjoying about the extreme Universe, Extreme Extreme, in which we

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Speaker 1: look at all the weirdest, nastiest, hottest, wettest, craziest things

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Speaker 1: in the universe, and we have actually done some of those.

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Speaker 1: We did the hottest, we did the brightest, we did

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Speaker 1: the biggest. What else did we do? You Ma, you

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Speaker 1: make our podcast sound a little not safe for work there, Daniel.

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Speaker 1: That's all in the minds of the listener. Okay, well,

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Speaker 1: that's that's kind of the universe totally. The universe is

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Speaker 1: not safe for work. Oh I thought you meant the

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Speaker 1: universe is in the minds of the listener, which is

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Speaker 1: also sort of true from a philosophical point of view.

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Speaker 1: So today we're continuing our series of extreme Things in

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Speaker 1: the universe, and in this episode we are going to

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Speaker 1: explore what is the dnsest thing in the universe, the

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Speaker 1: densest thing in the universe, that's right, Not the heaviest,

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Speaker 1: not the biggest, not the smallest, but the most compact,

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Speaker 1: the thing with the most stuffed stuffed into it, that's right,

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Speaker 1: Not the sharpest thing, the densest thing, that's right, Not

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Speaker 1: the brightest thing, but the densest things, right, Not the

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Speaker 1: smartest thing in the universe, the dances, that's right. Yeah,

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Speaker 1: the smartest thing in the universe. That would be an

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Speaker 1: interesting discussion. I wonder what is the smartest thing in

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Speaker 1: the universe. Do you think it's a human? Who? You

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Speaker 1: think it's some super intelligent alien race? I think the

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Speaker 1: universe is the smartest thing in the universe. Oh snap,

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Speaker 1: we are the universe thinking? Is that what you're thinking?

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Speaker 1: Where you're going? We are the brain of the universe.

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Speaker 1: The universe is us. It's very holistic of you. I

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Speaker 1: gotta get some of those banana peals you must have

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Speaker 1: been smoking for today's episode. I am one with the universe,

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Speaker 1: and the universe is me, and I am thinking the

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Speaker 1: thoughts of the universe. Well, I but I don't. I

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Speaker 1: don't smoke banana peals. I just I just eat them. Wrong,

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Speaker 1: You eat them, you eat the flesh, and I smoked

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Speaker 1: the peels. So we're a perfect team. Well, so, yeah,

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Speaker 1: what is the densest thing you meaning? Like, what is

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Speaker 1: the most compact crunched up think? Is you know, craziest

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Speaker 1: most amount of stuff in a small amount of space.

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Speaker 1: Thing that exists out there in the universe, that's right.

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Speaker 1: And the point of this series, the Extreme Universe series,

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Speaker 1: is to remind you that our little corner of the

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Speaker 1: universe is fairly ho hum. It's not very fast, it's

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Speaker 1: not very big, it's not very hot, it's not very cold.

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Speaker 1: It's sort of just right. And what that means is

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Speaker 1: that there is crazy stuff out there, this stuff out

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Speaker 1: there that's bigger you than you can imagine, that's hotter

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Speaker 1: than you can imagine, that's emptier than you can imagine.

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Speaker 1: And one of my funniest extremes is density. To imagine

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Speaker 1: how much stuff you can cram into the tiniest spot,

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Speaker 1: get those atoms all crowded up into each other. Because

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Speaker 1: when that happens, really weird things happen. Matter does all

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Speaker 1: sorts of strange stuff when you squeeze it together. And

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Speaker 1: so a lot of our listeners, a lot of you

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Speaker 1: listening out there, might be thinking, Oh, I know the

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Speaker 1: answer to this question. It's obviously a black hole. Hint,

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Speaker 1: it's not a black hole. It's not a black hole.

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Speaker 1: Maybe it is, maybe it isn't. There's a bit of

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Speaker 1: a philosophical argument there at the end teaser, there's a

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Speaker 1: plot twist. It is it isn't It is it isn't.

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Speaker 1: Some people say it is, some people say it isn't.

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Speaker 1: Those other people throw the other first people into a

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Speaker 1: black hole, and the argument and at all just becomes

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Speaker 1: a black hole of a mess exactly, it becomes a

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Speaker 1: mental black hole. We all get a little denser. So

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Speaker 1: hopefully that sucked you in into the topic of this podcast,

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Speaker 1: and so stay tuned to see if it is or

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Speaker 1: if it's not a black hole. Daniel says, maybe it

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Speaker 1: is not, Maybe it is, maybe it's not. Exactly, But

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Speaker 1: before we dive into that, I went around and I

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Speaker 1: asked folks on campus that you see Irvine. I said,

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Speaker 1: what do you think is the densest thing in the universe?

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Speaker 1: Because I was curious, is everybody just going to say

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Speaker 1: it's a black hole? To people have other ideas? Have

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Speaker 1: people done the careful reading about the fundamental issues in

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Speaker 1: the corners and the centers black holes? Or maybe people

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Speaker 1: knew what the densest thing in the universe is. Maybe

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Speaker 1: there it's it's something else and people knew about it. Yeah,

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Speaker 1: that's right. Maybe it's the center of some weird kind

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Speaker 1: of candy and you know, famously dance or something else

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Speaker 1: weird people have read about. So I walked around I

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Speaker 1: asked people. I said, what do you think is the

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Speaker 1: densest thing in the universe? So think about it for

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Speaker 1: a second, and if somebody asked you on the street,

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Speaker 1: what is the denist thing in the universe, would you

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Speaker 1: answer that it's a black hole. Here's what people had

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Speaker 1: to say. A black hole. Oh, man, I hope it's

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Speaker 1: chocolate black hole. Probably a black hole, a black hole,

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Speaker 1: neutron stars, something like that. Black holes gets the anti

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Speaker 1: matter black hole. I think I want to say the core,

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Speaker 1: the core core of the Earth, okay, okay, or actually,

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Speaker 1: so you know universe, probably the sun in the star, right, yeah,

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Speaker 1: I would say a star al right. So most people

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Speaker 1: answered black hole. A lot of people said it's a

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Speaker 1: black hole. It's a good go to thing. I think

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Speaker 1: people think what's the densest thing in the universe and

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Speaker 1: their mind goes straight to a black hole because they

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Speaker 1: imagine a black hole has a lot of stuff stuffed

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Speaker 1: into it. But it wasn't the only answer. There was

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Speaker 1: some pretty interesting ones here. I like the one that

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Speaker 1: said it's chocolate exactly. I'm not sure that was a

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Speaker 1: serious answer. Somebody out there really had a hanker and

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Speaker 1: for some dark, dark chocolate. Right. The thing that interested

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Speaker 1: me about these answers maybe they were thinking like richest,

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Speaker 1: Like what's the richest thing you've ever tasted? Most? What's

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Speaker 1: the most calorie dense thing in the universe? Maybe that's

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Speaker 1: what they're thinking. There you go, is it still a

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Speaker 1: black hole? Like what if you eat a black hole?

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Speaker 1: That's a lot of calories technically, right, what if you

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Speaker 1: ate a black hole? I think that's a physics question

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Speaker 1: nobody has ever asked me before. While we are breaking

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Speaker 1: new ground today. One of the things I liked about

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Speaker 1: these answers is in contrast to someone the other extreme

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Speaker 1: universe questions, where you you might have noticed people tended

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Speaker 1: to answer in their local environment. They're like, thought about

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Speaker 1: what is the brightest thing in our solar system? Or

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Speaker 1: what is the biggest thing nearby here? People really went

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Speaker 1: s at a universal They really cast their minds into

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Speaker 1: the entire universe to find something really really dense. I

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Speaker 1: mean like the person who said it was the core

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Speaker 1: of the earth exactly, not that person, everybody, but that

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Speaker 1: person yeah, all right, Well there were other answers here.

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Speaker 1: Some people said neutron stars, other people said antimatter. Those

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Speaker 1: are pretty a space physics the answers yeah, yeah, I

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Speaker 1: think antimatters a would have stabbed there. You know, Um,

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Speaker 1: antimatter is not anymore or less than the normal matter, right,

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Speaker 1: it's just another kind of matter. It's at the opposite

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Speaker 1: kind of matter. But a neutron star is a good answer. Um.

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Speaker 1: I like the people who said, you know, I don't

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Speaker 1: know something strange out there in space like that, you know,

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Speaker 1: just conveys the whole idea we're trying to get across here,

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Speaker 1: which is that space is filled with weird stuff, something

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Speaker 1: crazy and strange and you probably can't even imagine. Well,

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Speaker 1: that needs to be the answer to every single one

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Speaker 1: of these extreme universe episodes. It's like, what's the brightest

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Speaker 1: thing in the universe, some weird thing out there in space,

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Speaker 1: something in space. I've noticed this trend that you seem

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Speaker 1: to be trying to assemble a sort of universal list

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Speaker 1: of answers to physics questions, Like how many physics questions

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Speaker 1: can you just answer with the with the phrase the

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Speaker 1: Big bang or space or you know, physics. Um, it's

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Speaker 1: like you're trying to find shortcuts or something. Well, you know,

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Speaker 1: I want to be ready when that physicist approaches me

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Speaker 1: on the street wearing sandals and asking me strange questions

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Speaker 1: about the universe. I want to be ready. You know,

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Speaker 1: you want to be ready. I think we should do

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Speaker 1: that someday. We should just flip your answers in and

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Speaker 1: see if any listeners even noticed. Right, do I get

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Speaker 1: to Google first? Nobody gets to Google first. There's no

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Speaker 1: googling allowed in these questions. It's just what do you know? Now?

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Speaker 1: What's in your mind? What answer can you construct? All right, well,

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Speaker 1: let's launch into this discussion, Daniel. Let's figure out what

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Speaker 1: is the dancest thing in the universe. But first let's

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Speaker 1: maybe talk about what is density. I think we all

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Speaker 1: have an intuitive sense of what density is, but you know,

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Speaker 1: maybe there's a it's different from the physics definition. Yeah,

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Speaker 1: and we talk a lot in this podcast about sort

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Speaker 1: of the difference between technical physical definitions and sort of

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Speaker 1: cultural definitions, and in this one case, I think they're

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Speaker 1: pretty well aligned. But let's just go through the basics.

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Speaker 1: Being people up to speed in case they haven't thought

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Speaker 1: about density. Since you know high school chemistry or something

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Speaker 1: um And so density is not a fundamental unit, it's

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Speaker 1: a derived unit, which means it's a ratio of two

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Speaker 1: other things. It's mass over volume. So mass is just

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Speaker 1: like how much stuff is there. It's different from weight. Right, Wait,

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Speaker 1: is how much force is there on you from from

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Speaker 1: Earth's gravity. Mass is just like how much stuff is

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Speaker 1: there in you? Right, And remember we talked about that

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Speaker 1: another time. What is mass? And it comes from inertia

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Speaker 1: and it's the property of an object to resist changes

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Speaker 1: in its motion. Right, So that's what mass is. All

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Speaker 1: the particles inside you and all their energy addupt to

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Speaker 1: give you a certain amount of mass. And then on

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Speaker 1: the bottom of that volume, right, So it's mass over

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Speaker 1: a volume. And volume is just how much space do

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Speaker 1: you take up? Right? How big are you? So something

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Speaker 1: can be really dense if it has a lot of

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Speaker 1: mass and not very much volume, or not very much

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Speaker 1: mass but even less volume. Right. So it's not about

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Speaker 1: being extremes in mass or extremes in volume. It's all

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Speaker 1: about the ratio. It's having a lot of mass in

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Speaker 1: a small space. I see. It's not about being the

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Speaker 1: biggest thing or about having the most mass. It's about

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Speaker 1: having the most mass in the smallest amount of space. Yeah,

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Speaker 1: because you can think of things that are really really

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Speaker 1: big and really really massive, but not very dense, like

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Speaker 1: a blimp. Right. You know, a blimp is not that

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Speaker 1: dense because it can float in the air. Right, It's

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Speaker 1: filled with a gas that's less dense than air, even

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Speaker 1: though it's really big and uh and and it has

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Speaker 1: a huge amount of mass to it. A blimp is

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Speaker 1: not actually that dense. But if the blimp was made

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Speaker 1: out of rocks, that would be really really dense. That's right.

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Speaker 1: That would be a terrible design for a blimp exactly. Um,

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Speaker 1: I don't recommend you buy any stocks and your friends

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Speaker 1: rock blimp startup. Well, it depends on what you're trying

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Speaker 1: to float in, right, If you're trying to float into

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Speaker 1: something that is denser than rock, then they would work. Yeah,

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Speaker 1: that's true. I'm not sure where that exists, so you know,

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Speaker 1: he's lava denser than rock, probably not right, So I'm

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Speaker 1: not sure where your rock blimp would even work, but

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Speaker 1: sure yeah, maybe you know, on the surface sid maybe

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Speaker 1: in the liquid nitrogen oceans of Jupiter. There you go, there,

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Speaker 1: there you go. There's a great reason to invest in

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Speaker 1: your in that startup now. Yeah. But the point is,

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Speaker 1: things can be really big and really massive without being

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Speaker 1: very dense. Right. Dense requires a huge amount of mass

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Speaker 1: compacted into a small space. So the densest thing in

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Speaker 1: the universe doesn't have to be something big. It can

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Speaker 1: be something small, that's right. And things can be very

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Speaker 1: very dense without being that big. Right. You can have

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Speaker 1: a really really small amount of something that's very dense

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Speaker 1: as long as there's a huge amount of stuff crammed

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Speaker 1: into it. But it could also be a really big thing,

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Speaker 1: like you could you know, the densest thing in the

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Speaker 1: universe could be like a star or a neutron star.

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Speaker 1: It could be something that big. Yeah, exactly, it could

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Speaker 1: be big, it could be small. It could be massive,

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Speaker 1: it could be not that massive. The key is the

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Speaker 1: ratio again between the mass and the volume, how much

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Speaker 1: stuff is cramped into a certain amount of space exactly.

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Speaker 1: And you know, that's physics density, And I think that

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Speaker 1: matches pretty well with what people's intuition is for density.

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Speaker 1: I don't think we have a pretty big disconnect like

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Speaker 1: we usually do. So congratulation Physics Naming team. You picked

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Speaker 1: a good one this time. Well, I guess intuitively, you know,

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Speaker 1: it's kind of like, um, holding something in your hand.

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Speaker 1: You know, like if you're holding a little rock that's

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Speaker 1: dense and you know it's dnse because it feels heavy,

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Speaker 1: but it still fits in your hand. But if you

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Speaker 1: have you have like a ball of cotton in your hand,

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Speaker 1: that's not very dense, that's right. And so one way

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Speaker 1: to compare densities is to say, I'm going to compare

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Speaker 1: different kinds of stuff and have the same volume, so

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Speaker 1: the same amount of its same like physical space full

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Speaker 1: of it, and then just compare the mass because it's

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Speaker 1: the ratio of mass to volume. And if you fix

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Speaker 1: the volume, then you can just compare the mass us.

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Speaker 1: So you can compare like a handful of rock to

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Speaker 1: a handful of cotton, to a handful of air to

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Speaker 1: a handful of you know, hot lava or whatever. And

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Speaker 1: don't actually try to get a handful of hot lava,

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Speaker 1: but hand full of lava sounds like it sounds like

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Speaker 1: a you know, a high school band name or something

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Speaker 1: up next an extreme universe handful of lava. Anyway, Um, yeah,

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Speaker 1: you if you fix the volume, then you can compare

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Speaker 1: the mass. Okay, so you have a couple of great

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Speaker 1: interesting numbers here for us, and they're all based on

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Speaker 1: a fixed volume, which is a one teaspoon, right, that's right.

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Speaker 1: I thought a teaspoon is like a macroscopic quantity. You know,

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Speaker 1: you can imagine it's just like a normal kitchen spoonful

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Speaker 1: of stuff. And then we can think about how heavy,

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Speaker 1: how much mass is there in a teaspoon of this

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Speaker 1: versus a teaspoon of that versus the teaspoon of something else.

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Speaker 1: So if we fix the volume, then we can just

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Speaker 1: think about how much mass there is, how much a

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Speaker 1: teaspoon of something would Wait, that's right now. Wait, of

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Speaker 1: course is slightly different from mass, but you know they're connected.

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Speaker 1: And here Earth, something that has more mass has more weight. Um,

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Speaker 1: you know, far away from the Earth, then you can

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Speaker 1: still have mass even if you don't have weight. But

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Speaker 1: they're the same if we're if we're doing this experiment

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Speaker 1: on the surface of the Earth, then it's equivalent. So

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Speaker 1: step us through here, Daniel. All right, so I thought

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Speaker 1: we'd start really really light, all right, just sort of

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Speaker 1: for scale, and imagine if you had, for example, um,

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Speaker 1: a teaspoon of space right. I mean, I don't know

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Speaker 1: how you would get that, but so you like scooped

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Speaker 1: up a teaspoon of space, so you had, you know,

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Speaker 1: stuff that had the same density of space. Like what

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Speaker 1: do you mean space, like average space or like if

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Speaker 1: you win out into space, grabbed the scoop of it

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Speaker 1: and brought it back to Earth. Is that what you mean? Yeah?

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Speaker 1: The average amount the average amount of stuff in space.

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Speaker 1: And remember we did a whole podcast episode about how

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Speaker 1: space he is space and it turns out that the

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Speaker 1: answer is pretty different depending on where you get your

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Speaker 1: scoop of space. But in all cases, as long as

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Speaker 1: you're far away from the Earth's atmosphere, the answer is

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Speaker 1: pretty pretty low. You know, you're gonna get less than

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Speaker 1: one proton in your tea spoon. Okay, so this is

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Speaker 1: like the average teaspoon of the universe. Yeah, exactly. The

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Speaker 1: average density of a teaspoon in the universe is one

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Speaker 1: times ten to the negative twenty seven kilograms, So that's

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Speaker 1: zero point twenties seven. Zero's one. That's how much a proton. Ways,

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Speaker 1: so you can have like a whole teaspoon with just

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Speaker 1: a proton in it. That's about the average density of

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Speaker 1: stuff out there, and a proton is pretty small, right,

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Speaker 1: I mean it's it's pretty much. Uh, it's it's tiny.

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Speaker 1: It's almost nothing, right, it's almost a fundamental unit of

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Speaker 1: of mass. Right. Yeah, it's amazing because it's almost nothing.

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Speaker 1: But then it makes up everything, right, And it's incredible

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Speaker 1: how you can get big macroscopic stuff made out of

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Speaker 1: super tiny stuff. Right. It boggles the mind how small

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Speaker 1: a proton is, and then how many protons you need

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Speaker 1: to make, Like you know, a cookie or whatever. There's

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Speaker 1: so many protons in your cookie and you don't even

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Speaker 1: think about them as you eat it. Wow. So that's

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Speaker 1: the average density of the universe really, right, it's it's

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Speaker 1: about one proton per teaspoon. And the reason is, you know,

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Speaker 1: there's a lot of stuff out there in the universe,

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Speaker 1: a lot of stars and they're big, and a lot

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Speaker 1: of galaxies, but most of the universe is pretty empty,

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Speaker 1: you know, the stuff between stars and between galaxies. There's

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Speaker 1: not that much stuff there. And the biggest volume of

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Speaker 1: the universe are these super voids, you know, between the

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Speaker 1: sheets of superclusters. But there's really basically almost nothing. And

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Speaker 1: so because density is mass over volume, and the volume

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Speaker 1: of the universe is unbelievably gigantic. Then that's why the

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Speaker 1: density is so small. I mean, it's amazing that it's

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Speaker 1: even anywhere close to a proton. Frankly, Wow, that's pretty

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Speaker 1: incredible to think that if you sort of, like if

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Speaker 1: you shrank the entire universe into a teaspoon, like everything

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Speaker 1: that's stuff, stars as planets, would just be about the

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Speaker 1: size of a proton exactly. But but the next I thought,

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Speaker 1: let's let's look at something sort of around here on

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Speaker 1: the Earth, and and a good sort of normalization for

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Speaker 1: like a standard for what density is is water, because

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Speaker 1: water is one um gram per cubic centimeter, right, and

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Speaker 1: a teaspoon is five cubic centimeters, So water is five

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Speaker 1: grams per cubic centimeter. So you have a teaspoon of water,

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Speaker 1: it weighs five grams, which is a whole lot more

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Speaker 1: than a proton. What about a teaspoon of tea? A

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Speaker 1: teaspoon of tea, that's a good question. It must be

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Speaker 1: a little bit more dense, right because you put something

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Speaker 1: into it, but it's about the same, Okay, So that's um.

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Speaker 1: I think that's a pretty good anchor for people, maybe,

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Speaker 1: you know, because we're all sort of familiar with how

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Speaker 1: water feels and how much it wasgs. That's right, And

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Speaker 1: if you're holding a teaspoon, you can tell the difference

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Speaker 1: between having a full teaspoon and an empty teaspoon. Right,

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Speaker 1: somebody pours water into your teaspoon with your eyes closed,

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Speaker 1: you can tell the difference. Whereas if I put a

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Speaker 1: single proton in your teaspoon, you're not gonna notice. So

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Speaker 1: you can feel it, right, you can feel five grams.

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Speaker 1: It's not it's not a lot, but it's also not nothing.

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Speaker 1: That really kind of tells you how empty the universe is, right, Like,

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Speaker 1: if our average experience of matter is a teaspoon of water,

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Speaker 1: compare that to a teaspoon with one proton in it.

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Speaker 1: That's that's really kind of the difference between our everyday

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Speaker 1: experience and the actual whole other rest of the universe,

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Speaker 1: exactly at the low extreme, most of the universe is

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Speaker 1: really not very dense at all, So we live in

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Speaker 1: a pretty dense place compared to most of the universe.

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Speaker 1: But then again, as you'll hear, our surroundings are not

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Speaker 1: very dense at all compared to the densest places in

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Speaker 1: the universe, So The craziest thing about the universe is

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Speaker 1: that it has this enormous range. Most of it's not

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Speaker 1: very dense at all, and then there's these incredible pockets

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Speaker 1: of total density. Well, let's keep scooping up more and

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Speaker 1: more dens for things. But first let's take a quick break.

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Speaker 1: All right, we're scooping things up indiscriminately here and measuring

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Speaker 1: their density to find out the densest thing in the universe.

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Speaker 1: And we we just scipped up some water. So some

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Speaker 1: water is about five grams that's right, five grams per

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Speaker 1: tea spoon. And then people, um, a lot of people said, oh,

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Speaker 1: maybe the sun or a star. That seems like a

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Speaker 1: dense thing, right, because it seems like it's trapped by

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Speaker 1: gravity and the reason it's burning is that it's all

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Speaker 1: this gasp and compressed. So people figure, well, it must

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Speaker 1: be pretty dense, right, Well, it is dense, but it's

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Speaker 1: surprisingly not that dense. I mean, the density of the

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Speaker 1: sun is about seven grams per teaspoon, so only a

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Speaker 1: little bit denser than water. Are you serious? Yeah, the

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Speaker 1: sun is not that much denser than water. Yeah, the

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Speaker 1: Sun is not that much denser than the water. Now,

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Speaker 1: the sun is really big, and the Sun is really hot,

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Speaker 1: but it's not actually that dense. So this is the

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Speaker 1: average density of the Sun, because I imagine the Sun

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Speaker 1: is dens or at the middle in the middle unless

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Speaker 1: dense at the edges. Right, the Sun really doesn't like

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Speaker 1: when you talk about its middle that way. It's been

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Speaker 1: working on it for a few billion years um. But yes,

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Speaker 1: the the density of the Sun does vary. So this

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Speaker 1: is the average density exactly. And I think the reason

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Speaker 1: that it's not more dense is that there's more than

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Speaker 1: just gravity going on. Right. Gravity is the thing that

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Speaker 1: made the Sun. It pulled all that stuff together, it

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Speaker 1: starts that fire. But once you have that fire happening,

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Speaker 1: it's like a constant explosion, and that explosion is making

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Speaker 1: the Sun less dense. So the Sun is this constant balance, right,

424
00:21:18,240 --> 00:21:22,600
Speaker 1: It's a trapped, ongoing nuclear explosion. The explosions are pushing

425
00:21:22,600 --> 00:21:25,359
Speaker 1: things out and gravity is pulling things in. And so

426
00:21:25,480 --> 00:21:27,240
Speaker 1: if it was just gravity, then you know, the Sun

427
00:21:27,240 --> 00:21:30,359
Speaker 1: would collapse into a very very dense state. But the

428
00:21:30,400 --> 00:21:33,040
Speaker 1: reason it doesn't collapse is because it's exploding, so that

429
00:21:33,160 --> 00:21:35,120
Speaker 1: keeps it, you know, a little fluffy, So you're really

430
00:21:35,160 --> 00:21:38,520
Speaker 1: only kind of measuring the density of the fuel of

431
00:21:38,560 --> 00:21:41,520
Speaker 1: the sun, Like once it turns into fire and photons

432
00:21:42,000 --> 00:21:44,320
Speaker 1: once it turns into light, you don't really count that

433
00:21:44,400 --> 00:21:47,000
Speaker 1: as part of the density. That's right, we're measuring the

434
00:21:47,080 --> 00:21:49,400
Speaker 1: matter density of the sun. But you know a lot

435
00:21:49,440 --> 00:21:51,520
Speaker 1: of the photons produced in the sun never leave it

436
00:21:51,560 --> 00:21:54,040
Speaker 1: because they're reabsorbed. You make a photon somewhere in the

437
00:21:54,040 --> 00:21:56,280
Speaker 1: middle of the sun, it's going to get reabsorbed before

438
00:21:56,280 --> 00:21:58,080
Speaker 1: it leaves the sun. But I think they did is

439
00:21:58,080 --> 00:22:01,200
Speaker 1: that if you scooped up a teaspoon of the sun,

440
00:22:01,680 --> 00:22:03,600
Speaker 1: it would it would sort of feel the same as

441
00:22:03,600 --> 00:22:07,040
Speaker 1: this teaspoon of water. It might be a lot brighter, right,

442
00:22:07,080 --> 00:22:12,359
Speaker 1: and hotter, but exactly. Yeah, that's the idea, right, Somebody

443
00:22:12,400 --> 00:22:15,240
Speaker 1: out there is imagining being blindfolded, and you're saying, I'm

444
00:22:15,320 --> 00:22:17,520
Speaker 1: either going to pour a teaspoon of water into your

445
00:22:17,520 --> 00:22:19,879
Speaker 1: teaspoon or a teaspoon of the sun, and you won't

446
00:22:19,880 --> 00:22:22,000
Speaker 1: be able to tell which. And you're thinking, yeah, I

447
00:22:22,000 --> 00:22:24,560
Speaker 1: think I'll be able to tell. But you're right, you

448
00:22:24,600 --> 00:22:26,960
Speaker 1: won't be able to tell from the from the heaviness

449
00:22:27,000 --> 00:22:28,920
Speaker 1: of it, because it's not that much heavier than water,

450
00:22:29,040 --> 00:22:31,320
Speaker 1: all right, And in fact, it seems like things are

451
00:22:31,400 --> 00:22:33,800
Speaker 1: even denser here on Earth. Yeah, exactly. And you might

452
00:22:33,800 --> 00:22:35,680
Speaker 1: be thinking, well, water is not that dense, and you're right,

453
00:22:36,000 --> 00:22:38,639
Speaker 1: And if you just like bent down and scooped up

454
00:22:38,640 --> 00:22:41,800
Speaker 1: a teaspoon of rocks, you know of like gravel or whatever,

455
00:22:42,320 --> 00:22:44,600
Speaker 1: then you would have something denser. In fact, the density

456
00:22:44,640 --> 00:22:47,399
Speaker 1: of the Earth, again averaging over everything in the Earth,

457
00:22:47,720 --> 00:22:51,960
Speaker 1: is thirty grams per teaspoon. Remember waters five grams, the

458
00:22:52,000 --> 00:22:55,960
Speaker 1: sun is seven grams. The Earth is thirty grams per teaspoon.

459
00:22:56,080 --> 00:22:58,280
Speaker 1: That's a lot denser than the Sun. So the Sun

460
00:22:58,359 --> 00:23:01,520
Speaker 1: is actually kind of fluffy, right, Yeah, it's like a

461
00:23:01,520 --> 00:23:04,919
Speaker 1: big cozy pillow on fire. Yeah. And the reason is right,

462
00:23:04,920 --> 00:23:08,280
Speaker 1: the Earth is not on fire. Right. If the Earth

463
00:23:09,080 --> 00:23:12,040
Speaker 1: was more massive so that there was more gravity so

464
00:23:12,080 --> 00:23:14,679
Speaker 1: we can press it more infusion would get started, then

465
00:23:14,720 --> 00:23:17,080
Speaker 1: it would actually get bigger, right, and then it would

466
00:23:17,080 --> 00:23:19,879
Speaker 1: be more fluffy. So Earth is more dense because we

467
00:23:19,960 --> 00:23:22,560
Speaker 1: only have gravity going on. We have no outward pressure

468
00:23:22,920 --> 00:23:25,760
Speaker 1: from fusion to make us fluffy. We're not living in

469
00:23:25,800 --> 00:23:29,720
Speaker 1: an explosion. We are pretty compact. So but that's kind

470
00:23:29,720 --> 00:23:33,360
Speaker 1: of the average density of the Earth. But there must

471
00:23:33,400 --> 00:23:36,520
Speaker 1: be things on Earth that are denser than the average density.

472
00:23:36,640 --> 00:23:38,840
Speaker 1: Big variation in density. You know, the core of the

473
00:23:38,920 --> 00:23:41,280
Speaker 1: Earth is more dense than the rocks under your feet,

474
00:23:41,280 --> 00:23:44,680
Speaker 1: for example. So there's a lot of variation. But if

475
00:23:44,680 --> 00:23:46,600
Speaker 1: you look around on Earth, for like, what is the

476
00:23:46,680 --> 00:23:49,840
Speaker 1: densest thing that occurs on Earth? There's this one element

477
00:23:49,840 --> 00:23:53,800
Speaker 1: it's called osmy um, and osmium weighs a hundred ten

478
00:23:53,960 --> 00:23:58,119
Speaker 1: grams per teaspoon a hundred and ten grams, so like, um,

479
00:23:58,160 --> 00:24:01,720
Speaker 1: that's a lot. That's like, how much is that like

480
00:24:01,840 --> 00:24:07,320
Speaker 1: fifteen scoops of the sun compressed down? Is how much

481
00:24:07,400 --> 00:24:11,440
Speaker 1: osm that's right? Um, If you had a teaspoon of osmium,

482
00:24:11,520 --> 00:24:13,439
Speaker 1: it would feel like you had like a half a

483
00:24:13,440 --> 00:24:16,679
Speaker 1: cup of water in your teaspoon. The stuff is pretty dense.

484
00:24:16,880 --> 00:24:18,480
Speaker 1: I've never seen ausman. I don't even know what it

485
00:24:18,480 --> 00:24:20,320
Speaker 1: looks like or if you can pour it, if it's

486
00:24:20,320 --> 00:24:23,480
Speaker 1: liquided room temperature or whatever. But it's the densest stuff

487
00:24:23,480 --> 00:24:25,960
Speaker 1: on Earth. But that's at the on the surface of

488
00:24:26,000 --> 00:24:28,880
Speaker 1: the Earth. Like maybe down in the center of the Earth,

489
00:24:28,880 --> 00:24:31,639
Speaker 1: things are more compact because there's more pressure. Yeah, and

490
00:24:31,680 --> 00:24:34,320
Speaker 1: you're right, the core of the Earth is more dense

491
00:24:34,359 --> 00:24:36,240
Speaker 1: than the rest of the Earth or the Earth's crust

492
00:24:36,280 --> 00:24:38,480
Speaker 1: for example, or the average density of the Earth, which

493
00:24:38,520 --> 00:24:41,160
Speaker 1: is what we mentioned earlier. But sort of surprisingly, it's

494
00:24:41,160 --> 00:24:44,000
Speaker 1: not that much more dense, Like it's twice as dense

495
00:24:44,080 --> 00:24:45,840
Speaker 1: at the core of the Earth than it is at

496
00:24:45,840 --> 00:24:48,359
Speaker 1: the Earth's crust, which is most of the Earth. But

497
00:24:48,560 --> 00:24:51,119
Speaker 1: so it's not crazy. It's not like a jillion times

498
00:24:51,160 --> 00:24:53,320
Speaker 1: denser or anything. I mean, twice as dance is a lot,

499
00:24:53,359 --> 00:24:55,679
Speaker 1: but it's not. It's not shocking. Okay, So now take

500
00:24:55,760 --> 00:24:57,800
Speaker 1: us out into space, Daniel, what are some of the

501
00:24:57,840 --> 00:25:00,879
Speaker 1: densest things out there in space? Well, so, as we

502
00:25:00,920 --> 00:25:04,200
Speaker 1: talked about, stars that are normally burning, are not actually

503
00:25:04,240 --> 00:25:07,399
Speaker 1: that dense, right, and so in our solar they're pretty fluffy.

504
00:25:07,400 --> 00:25:09,480
Speaker 1: In our Solar system, one of the densest things is

505
00:25:09,560 --> 00:25:13,160
Speaker 1: just the Earth, right, It's a pretty concentrated blob of rock.

506
00:25:13,400 --> 00:25:15,080
Speaker 1: So what you gotta do if you want something really

507
00:25:15,119 --> 00:25:17,639
Speaker 1: dense is something I think one of our listeners on

508
00:25:17,680 --> 00:25:19,919
Speaker 1: the street or one of our interviewees on the street

509
00:25:19,920 --> 00:25:22,600
Speaker 1: actually mentioned what you need is a failed star or

510
00:25:22,640 --> 00:25:25,880
Speaker 1: a star that has gone supernova and then collapsed, right.

511
00:25:26,560 --> 00:25:29,760
Speaker 1: And sometimes when a star blows its load, and it's

512
00:25:29,760 --> 00:25:32,679
Speaker 1: finished burning all of its fuel and it's expended all

513
00:25:32,680 --> 00:25:35,520
Speaker 1: of its energy, and that it no longer has that

514
00:25:35,640 --> 00:25:38,720
Speaker 1: radiation pressure to keep it fluffy. It collapses into a

515
00:25:38,800 --> 00:25:42,960
Speaker 1: neutron star. It's called a neutron star because the the

516
00:25:43,000 --> 00:25:46,399
Speaker 1: gravity is so intense that it forces all the protons

517
00:25:46,440 --> 00:25:48,880
Speaker 1: to give off an electron and become neutrons. And it's

518
00:25:48,920 --> 00:25:52,040
Speaker 1: just like a big ball of neutrons and they are

519
00:25:52,200 --> 00:25:54,840
Speaker 1: really scrunched in together, right, because there's so many of

520
00:25:54,840 --> 00:25:58,639
Speaker 1: them that the gravity really compresses things and makes it really,

521
00:25:58,680 --> 00:26:02,359
Speaker 1: really really dense. That's it. It's ridiculously dense because again

522
00:26:02,359 --> 00:26:05,280
Speaker 1: there's no process going on to counteract is, so all

523
00:26:05,359 --> 00:26:07,320
Speaker 1: you have is gravity. Is just like packing these little

524
00:26:07,359 --> 00:26:10,960
Speaker 1: neutrons and imagine like a huge bag of ping pong balls, right,

525
00:26:11,000 --> 00:26:13,359
Speaker 1: and you squeeze it so that they find like every

526
00:26:13,400 --> 00:26:15,640
Speaker 1: little gap of space gets squeezed out, and they all

527
00:26:15,680 --> 00:26:18,480
Speaker 1: find exactly the tightest way they can all fit together.

528
00:26:19,040 --> 00:26:21,199
Speaker 1: And the density of this thing is incredible. I mean,

529
00:26:21,240 --> 00:26:23,600
Speaker 1: it's even hard to understand. You know, we're talking about

530
00:26:23,600 --> 00:26:26,800
Speaker 1: a teaspoon. If you had a teaspoon of a neutron star,

531
00:26:27,280 --> 00:26:31,360
Speaker 1: it would be fifty times ten to the eleven kilograms.

532
00:26:32,359 --> 00:26:34,680
Speaker 1: That's a lot of eleven Yeah, exactly. I think that's

533
00:26:34,760 --> 00:26:38,840
Speaker 1: five thousand billion kilograms per teaspoon. And you rode here,

534
00:26:38,880 --> 00:26:43,159
Speaker 1: it's about seven hundred thousand Eiffel towers in a single

535
00:26:43,160 --> 00:26:45,680
Speaker 1: tea spoon. Yeah. I was trying to find an understandable

536
00:26:45,760 --> 00:26:49,439
Speaker 1: unit of of mass, like you know, what is comparable

537
00:26:49,440 --> 00:26:52,080
Speaker 1: in mass to a teaspoon of a neutron star. And

538
00:26:52,160 --> 00:26:55,280
Speaker 1: it turns out, you know, it's almost a million Eiffel

539
00:26:55,280 --> 00:26:58,000
Speaker 1: towers boiled down into a tea spoon. Like, I mean,

540
00:26:58,040 --> 00:27:00,240
Speaker 1: it's ridiculous, Like you couldn't hold up a sing the

541
00:27:00,280 --> 00:27:02,600
Speaker 1: Eiffel Tower. I mean, I know you've been working out

542
00:27:02,600 --> 00:27:04,840
Speaker 1: and you're pretty strong and everything, but an Eiffel tower

543
00:27:04,880 --> 00:27:07,439
Speaker 1: weighs a lot. Now I take a million Eiffel towers

544
00:27:07,560 --> 00:27:10,400
Speaker 1: and then condense them down into a tiny teaspoon, It's

545
00:27:10,400 --> 00:27:13,000
Speaker 1: hard to even imagine what that kind of matter is. Like,

546
00:27:13,320 --> 00:27:17,919
Speaker 1: what you know I am stronger in France is that

547
00:27:17,960 --> 00:27:19,960
Speaker 1: because the Earth is not round, there's a difference in

548
00:27:20,000 --> 00:27:22,600
Speaker 1: like the difference from the distance from the center of

549
00:27:22,640 --> 00:27:25,240
Speaker 1: the Earth. It's probably just the French wines out there.

550
00:27:26,400 --> 00:27:34,040
Speaker 1: You feel stronger in France. Exactly, But I think I

551
00:27:34,080 --> 00:27:36,680
Speaker 1: see what you're saying is that, like a neutron start

552
00:27:36,760 --> 00:27:39,119
Speaker 1: is really just a star that went out right, or

553
00:27:39,160 --> 00:27:41,840
Speaker 1: that collapse, Yeah, exactly, it finished burning. And so you're

554
00:27:41,840 --> 00:27:45,160
Speaker 1: saying that, like our son would be that dense, except

555
00:27:45,200 --> 00:27:49,440
Speaker 1: that since it's exploding, it kind of keeps everything fluffy.

556
00:27:49,600 --> 00:27:51,520
Speaker 1: But if you were to suddenly turn it off, all

557
00:27:51,560 --> 00:27:55,320
Speaker 1: that stuff woulds crunched down into something like a neutron star. Right.

558
00:27:55,400 --> 00:27:57,520
Speaker 1: And so to take the bomb analogy, you know, a

559
00:27:57,600 --> 00:28:01,080
Speaker 1: nuclear bomb when it's exploded is not actually that dense.

560
00:28:01,119 --> 00:28:03,520
Speaker 1: It's a huge fireball, right, But the fireball itself is

561
00:28:03,560 --> 00:28:06,800
Speaker 1: not that dense. It's much more dense before it explodes, right,

562
00:28:06,840 --> 00:28:09,359
Speaker 1: when it has all that fuel compacted into a small place.

563
00:28:10,000 --> 00:28:13,200
Speaker 1: After it explodes, it's much less dense. So an exploding

564
00:28:13,240 --> 00:28:15,840
Speaker 1: bomb is less dense than a non exploding bomb. Right.

565
00:28:15,840 --> 00:28:17,960
Speaker 1: It's kind of like can candy. You know how can

566
00:28:18,040 --> 00:28:21,840
Speaker 1: candy is big and fluffy, but if you like crunch

567
00:28:21,920 --> 00:28:24,960
Speaker 1: it down, then you just get one really dense piece

568
00:28:24,960 --> 00:28:28,600
Speaker 1: of candy. Yeah, you're making, uh, the sun sound really

569
00:28:28,640 --> 00:28:32,159
Speaker 1: comfortable and cozy. It's like big and fluffy like cotton candy.

570
00:28:32,320 --> 00:28:37,720
Speaker 1: You know, every pink pink? What is in the air

571
00:28:37,760 --> 00:28:40,240
Speaker 1: over your house that you think the sun is pink? Well,

572
00:28:40,280 --> 00:28:43,360
Speaker 1: you know that it depends on your If you're wearing

573
00:28:43,800 --> 00:28:47,200
Speaker 1: a rose color glasses, you know, I'll give it to you.

574
00:28:47,240 --> 00:28:51,480
Speaker 1: That's your cartoonist license, you know, that's your art um. Yeah, exactly.

575
00:28:51,480 --> 00:28:54,040
Speaker 1: So a neutron star is actually one of the densest

576
00:28:54,040 --> 00:28:57,360
Speaker 1: things in the universe. It's it's unbelievably dense. You know,

577
00:28:57,400 --> 00:29:00,240
Speaker 1: I think isn't even denser than Thor's hammer. You're the

578
00:29:00,240 --> 00:29:04,200
Speaker 1: Marvel Universe guy. I think it is. It is made

579
00:29:04,360 --> 00:29:08,880
Speaker 1: from the heart of a dying neutron star. So I

580
00:29:08,920 --> 00:29:12,160
Speaker 1: don't know if it's heavier, but it sounds like it's

581
00:29:12,160 --> 00:29:14,320
Speaker 1: maybe in the same order of magnitude. Well, so then

582
00:29:14,320 --> 00:29:17,400
Speaker 1: do the calculation. You know, if a teaspoon of neutron

583
00:29:17,480 --> 00:29:21,200
Speaker 1: star is a million Eiffel towers, then Thor's hammer is what,

584
00:29:21,360 --> 00:29:24,880
Speaker 1: I don't know, a hundred teaspoons, a thousand teaspoons. You know,

585
00:29:24,920 --> 00:29:28,120
Speaker 1: you're talking a billion Eiffel towers. So every time Thorpe

586
00:29:28,160 --> 00:29:31,280
Speaker 1: picks up that hammer, he's lifting a billion Eiffel towers.

587
00:29:31,440 --> 00:29:36,920
Speaker 1: It's a calming book. Wait, we're doing the physics of

588
00:29:36,920 --> 00:29:39,680
Speaker 1: comic books here today, folks. Um. Yeah, but you know,

589
00:29:39,840 --> 00:29:41,600
Speaker 1: not only do you have to be strong, but you

590
00:29:41,600 --> 00:29:44,200
Speaker 1: have to be worthy right to pick up Thor's hammer.

591
00:29:44,600 --> 00:29:47,680
Speaker 1: So so that's pretty dense. If you scoop up some

592
00:29:47,800 --> 00:29:50,720
Speaker 1: neutron star in a teaspoon, you would be picking up

593
00:29:51,080 --> 00:29:53,800
Speaker 1: a million Eiffel towers. Yeah, so make sure you do

594
00:29:53,880 --> 00:29:56,200
Speaker 1: your stretches before you try that, or you're gonna hurt yourself.

595
00:29:56,480 --> 00:30:00,760
Speaker 1: Make sure you use a strong spoon. Boon made out

596
00:30:00,800 --> 00:30:03,920
Speaker 1: of osmium, or a spoon made out of a billion

597
00:30:04,000 --> 00:30:11,800
Speaker 1: Eiffel towers, that's right, or vibranium. You sort of give

598
00:30:11,840 --> 00:30:13,880
Speaker 1: it away. You said a neutron star is one of

599
00:30:13,920 --> 00:30:16,600
Speaker 1: the densest things in the universe. But maybe so you're

600
00:30:16,600 --> 00:30:18,760
Speaker 1: saying it's not the densest thing. Well, it's it's a

601
00:30:18,760 --> 00:30:21,960
Speaker 1: little bit unclear. Depends a little bit who's camp you're in.

602
00:30:22,760 --> 00:30:25,200
Speaker 1: Are you an Einstein kind of person or are you

603
00:30:25,240 --> 00:30:28,080
Speaker 1: a shorting Your kind of person, Because depending on what

604
00:30:28,120 --> 00:30:30,960
Speaker 1: you think is going on inside a black hole, black

605
00:30:31,000 --> 00:30:33,960
Speaker 1: holes are either the densest thing in the universe or

606
00:30:34,120 --> 00:30:36,960
Speaker 1: not very dense at all. All right time to pick

607
00:30:37,080 --> 00:30:41,880
Speaker 1: sides Einstein versus short Anger. But first let's take a

608
00:30:41,960 --> 00:30:57,400
Speaker 1: quick break. All right, we're talking about the densest thing

609
00:30:57,400 --> 00:31:00,720
Speaker 1: in the universe, and we got to we are now

610
00:31:00,760 --> 00:31:04,480
Speaker 1: at um black holes. That's right, and we are right

611
00:31:04,520 --> 00:31:07,920
Speaker 1: smack in the middle of the longest standing physics grudge match.

612
00:31:08,400 --> 00:31:13,880
Speaker 1: It's general relativity versus quantum mechanics, Albert Einstein versus Schrodinger

613
00:31:14,000 --> 00:31:17,400
Speaker 1: in Heisenberg and all those other smart folks. And so

614
00:31:18,120 --> 00:31:20,040
Speaker 1: you might be thinking that there are Let's tell me

615
00:31:20,040 --> 00:31:22,160
Speaker 1: how dance is a black hole, because a black hole

616
00:31:22,280 --> 00:31:24,880
Speaker 1: is also something that happens after a star collapses. Right,

617
00:31:25,160 --> 00:31:27,760
Speaker 1: Sometimes the star performs a neutron star. Sometimes it forms

618
00:31:27,760 --> 00:31:29,920
Speaker 1: a black hole. And a black hole seems like it

619
00:31:30,000 --> 00:31:32,200
Speaker 1: must be the densest thing in the universe because it

620
00:31:32,240 --> 00:31:36,040
Speaker 1: has the strongest gravity. Right. The problem with the black

621
00:31:36,080 --> 00:31:38,520
Speaker 1: hole is that how do you define the edge of

622
00:31:38,560 --> 00:31:41,240
Speaker 1: the black hole? Remember that to talk about density, we

623
00:31:41,240 --> 00:31:43,960
Speaker 1: have to talk about mass. Black holes have huge masses,

624
00:31:44,320 --> 00:31:47,680
Speaker 1: but we also have to talk about volume. So what's

625
00:31:47,720 --> 00:31:50,360
Speaker 1: the denominator? What's the edge of the black hole? And

626
00:31:50,360 --> 00:31:53,080
Speaker 1: one very reasonable thing to say is that the edge

627
00:31:53,080 --> 00:31:55,360
Speaker 1: of the black hole is the point of no return,

628
00:31:55,720 --> 00:31:58,000
Speaker 1: you know, the point where if you're closer to the

629
00:31:58,040 --> 00:32:00,320
Speaker 1: center of the black hole than that than light can't

630
00:32:00,400 --> 00:32:03,200
Speaker 1: escape and nothing can never leave. Right, So you're sort

631
00:32:03,200 --> 00:32:06,240
Speaker 1: of saying, how do you when what do you count

632
00:32:06,240 --> 00:32:08,640
Speaker 1: as the black hole? Is the question exactly, because if

633
00:32:08,640 --> 00:32:11,840
Speaker 1: you're gonna do density, you have to calculate mass over volume.

634
00:32:12,120 --> 00:32:14,920
Speaker 1: So what volume are you including? So you're saying, one

635
00:32:14,920 --> 00:32:18,880
Speaker 1: option is to use what they call the event horizon, right, right,

636
00:32:19,120 --> 00:32:23,120
Speaker 1: the point where not even light can escape the vicinity

637
00:32:23,160 --> 00:32:25,040
Speaker 1: of the black hole. That's right, And I think that's

638
00:32:25,040 --> 00:32:28,800
Speaker 1: a reasonable definition because we can't see inside the event horizons.

639
00:32:28,840 --> 00:32:31,720
Speaker 1: We have no idea what's going on inside the event horizon,

640
00:32:31,960 --> 00:32:34,920
Speaker 1: so all we really can do is average over it. Right,

641
00:32:34,960 --> 00:32:37,000
Speaker 1: we can say, well, we know how much mass there is,

642
00:32:37,000 --> 00:32:39,320
Speaker 1: and we know how big it is, what's going on inside?

643
00:32:39,520 --> 00:32:42,040
Speaker 1: You know, that's Einstein versus Shortinger. So if you don't

644
00:32:42,040 --> 00:32:44,959
Speaker 1: want to be dependent on which physics genius is right

645
00:32:45,000 --> 00:32:47,920
Speaker 1: about the universe, then you just need to calculate the

646
00:32:47,920 --> 00:32:51,200
Speaker 1: mass the black hole divided by the volume includes enclosed

647
00:32:51,200 --> 00:32:53,480
Speaker 1: by that event horizon. So I think you're saying that

648
00:32:53,560 --> 00:32:57,400
Speaker 1: a black hole should be measured by when it's when

649
00:32:57,440 --> 00:33:00,440
Speaker 1: it's black. Yeah, exactly when the black star like that

650
00:33:01,280 --> 00:33:05,760
Speaker 1: where the black star and the whole holiness. That's right.

651
00:33:06,360 --> 00:33:09,160
Speaker 1: And the issue with black holes then is that they

652
00:33:09,160 --> 00:33:11,680
Speaker 1: are really really massive, right, which means it's a huge

653
00:33:11,680 --> 00:33:14,920
Speaker 1: amount of gravity, which means the event horizon is really

654
00:33:14,920 --> 00:33:17,959
Speaker 1: really big. So you say, you don't know what's going

655
00:33:18,000 --> 00:33:19,640
Speaker 1: on inside a black hole, but there's a huge amount

656
00:33:19,640 --> 00:33:23,560
Speaker 1: of mass in there. The event horizon grows linearly with mass.

657
00:33:23,560 --> 00:33:26,320
Speaker 1: So for example, you have twice as much mass, the

658
00:33:26,360 --> 00:33:29,720
Speaker 1: event horizon is twice as big. It's it's it's linear.

659
00:33:29,800 --> 00:33:32,360
Speaker 1: It's like a it's like a one to one increase.

660
00:33:33,120 --> 00:33:35,840
Speaker 1: I give you double the mass exactly. You double the

661
00:33:35,960 --> 00:33:39,800
Speaker 1: radius of the of the black area exactly. You double

662
00:33:39,880 --> 00:33:42,600
Speaker 1: the radius of the event horizon. Now, for those of

663
00:33:42,640 --> 00:33:45,560
Speaker 1: you you know something about geometry, think about that sphere

664
00:33:45,720 --> 00:33:47,959
Speaker 1: right now. If you double the radius of the sphere,

665
00:33:48,280 --> 00:33:50,440
Speaker 1: how much does the volume go up? Well, it goes

666
00:33:50,520 --> 00:33:53,880
Speaker 1: up like the radius cubed. Right. So, so you have

667
00:33:53,920 --> 00:33:57,840
Speaker 1: some black hole and you double its mass somehow, then

668
00:33:57,960 --> 00:34:01,560
Speaker 1: you've increased its mass by two, but you've increased its

669
00:34:01,680 --> 00:34:05,480
Speaker 1: volume by eight. Right, two cubed, so the density actually

670
00:34:05,520 --> 00:34:08,600
Speaker 1: goes down. So you double the mass of a black hole,

671
00:34:08,800 --> 00:34:11,759
Speaker 1: it's density goes down by a factor of four, which

672
00:34:11,840 --> 00:34:14,799
Speaker 1: means really really massive according to your definition of the

673
00:34:14,920 --> 00:34:17,560
Speaker 1: of the black holes, if you count the black part

674
00:34:17,640 --> 00:34:19,640
Speaker 1: as the black hole exactly, which seems like a reasonable

675
00:34:19,640 --> 00:34:21,960
Speaker 1: definition though you know, we'll talk about another definition in

676
00:34:22,000 --> 00:34:24,279
Speaker 1: a moment. And so what that means is that the

677
00:34:24,360 --> 00:34:27,080
Speaker 1: bigger your black hole is, sorry, the more massive your

678
00:34:27,080 --> 00:34:30,040
Speaker 1: black hole is, the less dense it actually is. But

679
00:34:30,200 --> 00:34:33,040
Speaker 1: you know, I guess it's a your I see what

680
00:34:33,080 --> 00:34:35,000
Speaker 1: you're saying, like that you should count the black as

681
00:34:35,000 --> 00:34:40,279
Speaker 1: the black hole. But that's it's not like a physical boundary,

682
00:34:40,400 --> 00:34:42,600
Speaker 1: you know, And it's not like it's not like a surface,

683
00:34:42,640 --> 00:34:44,080
Speaker 1: do you know what I mean. It's just where the

684
00:34:44,120 --> 00:34:48,040
Speaker 1: effect of the gravity starts to get crazy, but it's

685
00:34:48,080 --> 00:34:50,120
Speaker 1: not really sort of like you can't really touch the

686
00:34:50,160 --> 00:34:54,840
Speaker 1: surface of the black part, right. I wouldn't recommend it, um,

687
00:34:54,920 --> 00:34:57,480
Speaker 1: but you know, it is a real physical boundary. You know,

688
00:34:57,520 --> 00:35:00,319
Speaker 1: if you're a photon and you are pro do that

689
00:35:00,400 --> 00:35:02,520
Speaker 1: and you don't turn, you're gonna fall in. You know.

690
00:35:02,600 --> 00:35:04,640
Speaker 1: It's like saying, how big is the Grand Canyon. While

691
00:35:04,680 --> 00:35:07,239
Speaker 1: you start the definition at the edge of the Grand Canyon, right,

692
00:35:07,280 --> 00:35:09,360
Speaker 1: not at the not at the river at the bottom

693
00:35:09,360 --> 00:35:11,719
Speaker 1: of it. That made that Grand canyon. Right, you fall

694
00:35:11,719 --> 00:35:13,680
Speaker 1: in the Grand Canyon, you still fell in the Grand Canyon.

695
00:35:13,719 --> 00:35:15,200
Speaker 1: It doesn't matter if you fall into the edge or

696
00:35:15,200 --> 00:35:16,840
Speaker 1: if you jump out of a helicopter in the middle.

697
00:35:17,440 --> 00:35:19,879
Speaker 1: So I think it's a pretty reasonable definition that you're

698
00:35:20,040 --> 00:35:23,600
Speaker 1: you're putting the emphasis on the whole part. Well, that's

699
00:35:23,760 --> 00:35:25,759
Speaker 1: what makes the black hole so cool, right, is the

700
00:35:25,800 --> 00:35:27,920
Speaker 1: whole part, not the black part. So if you just

701
00:35:27,960 --> 00:35:30,359
Speaker 1: think of it the black hole as a whole, then

702
00:35:30,400 --> 00:35:33,680
Speaker 1: you have to measure where the whole starts. Yeah, so

703
00:35:33,719 --> 00:35:36,600
Speaker 1: you're saying them the density of the black hole, not

704
00:35:36,719 --> 00:35:39,880
Speaker 1: determined by how much mass is inside of the black hole,

705
00:35:40,040 --> 00:35:41,759
Speaker 1: is just kind of like how big the hole is,

706
00:35:42,040 --> 00:35:45,040
Speaker 1: which when it grows, it doesn't help the density, that's right,

707
00:35:45,040 --> 00:35:47,759
Speaker 1: because it's a connection there. Right. The more mass, the

708
00:35:47,800 --> 00:35:51,239
Speaker 1: bigger the hole, and the bigger the whole, the less dense, right,

709
00:35:51,320 --> 00:35:53,839
Speaker 1: So you sort of trapped there. In fact, to get

710
00:35:53,840 --> 00:35:55,880
Speaker 1: a really dense black hole, what you need to do

711
00:35:55,960 --> 00:35:59,920
Speaker 1: is is have um a smaller black hole. Right, If

712
00:36:00,040 --> 00:36:02,439
Speaker 1: you take half of the mass away from the black hole,

713
00:36:02,480 --> 00:36:05,040
Speaker 1: which of course you can't do, right, Then the mass

714
00:36:05,080 --> 00:36:08,200
Speaker 1: goes down by two, but the volume goes down by eight.

715
00:36:08,440 --> 00:36:12,080
Speaker 1: And so now the density increases by a factor of four. Okay,

716
00:36:12,120 --> 00:36:16,000
Speaker 1: so then the smaller the black hole, the denser it is. Yes, exactly,

717
00:36:16,080 --> 00:36:18,560
Speaker 1: So start with like a really big black hole, right.

718
00:36:19,080 --> 00:36:21,239
Speaker 1: I did some some calculations here. If you have a

719
00:36:21,320 --> 00:36:24,640
Speaker 1: supermassive black hole that has like the mass of four

720
00:36:24,800 --> 00:36:28,719
Speaker 1: billion sons, right, four billion times the mass of our Sun,

721
00:36:28,840 --> 00:36:32,160
Speaker 1: would be really really big black hole. It's event horizon

722
00:36:32,200 --> 00:36:34,640
Speaker 1: would be so big that the density of the black

723
00:36:34,640 --> 00:36:37,759
Speaker 1: hole would be the same as water, be five grams

724
00:36:38,120 --> 00:36:40,719
Speaker 1: per teaspoon of black hole. Oh, I see, because all

725
00:36:40,760 --> 00:36:46,120
Speaker 1: the masses just concentrated inside of this really really big hole. Exactly.

726
00:36:46,120 --> 00:36:48,360
Speaker 1: And again we're saying we don't know where stuff is

727
00:36:48,360 --> 00:36:50,920
Speaker 1: inside the hole. You know, we'll talk about that in

728
00:36:50,920 --> 00:36:53,360
Speaker 1: a moment. But if you have a really really dense

729
00:36:53,440 --> 00:36:56,120
Speaker 1: blob of matter that forms a black hole, then it's

730
00:36:56,120 --> 00:36:59,160
Speaker 1: event horizing is so big that it's really on average

731
00:36:59,560 --> 00:37:04,040
Speaker 1: on it's not denser than the water. Do you see

732
00:37:04,080 --> 00:37:06,640
Speaker 1: them unsatisfied by that? Well, I'm just confused a little bit.

733
00:37:06,680 --> 00:37:09,040
Speaker 1: So you're saying it's it's you need a billion sons

734
00:37:09,120 --> 00:37:12,319
Speaker 1: for this, right, four billion sons. Four billion sons. So

735
00:37:12,360 --> 00:37:15,000
Speaker 1: if you stuck four billion sons inside of a sphere

736
00:37:15,440 --> 00:37:18,799
Speaker 1: that big, it would be a black hole. It would

737
00:37:18,800 --> 00:37:20,600
Speaker 1: be a black hole. It doesn't matter how those sons

738
00:37:20,600 --> 00:37:23,040
Speaker 1: are arranged inside. It could be in a little point

739
00:37:23,040 --> 00:37:26,160
Speaker 1: in the middle, or it could be in a you know,

740
00:37:26,239 --> 00:37:28,880
Speaker 1: the form of unicorns spread all over the whole. It

741
00:37:28,880 --> 00:37:31,319
Speaker 1: would still create the same black hole. They could spell

742
00:37:31,320 --> 00:37:34,439
Speaker 1: out your name absolutely. So you're saying that we don't

743
00:37:34,440 --> 00:37:37,840
Speaker 1: know what the mass, how the mass is distributed inside

744
00:37:37,840 --> 00:37:40,759
Speaker 1: of that black sphere. It could be anything that's right,

745
00:37:41,239 --> 00:37:43,640
Speaker 1: and we don't because we can't see inside black holes.

746
00:37:43,640 --> 00:37:46,080
Speaker 1: So we don't know what the distribution of mass is.

747
00:37:46,080 --> 00:37:48,000
Speaker 1: Is it all in one little point in the center.

748
00:37:48,520 --> 00:37:51,840
Speaker 1: Is it a little fuzzier because the quantum mechanics is

749
00:37:51,880 --> 00:37:55,320
Speaker 1: it's some broader distribution. We don't know because we can't see.

750
00:37:55,640 --> 00:37:58,239
Speaker 1: That's why it's a reasonable definition to say, you know

751
00:37:58,280 --> 00:38:01,320
Speaker 1: everything inside this sphere, because we can't see any deeper anyway.

752
00:38:01,360 --> 00:38:04,560
Speaker 1: Anything beyond that requires speculation. I always thought black holes

753
00:38:04,600 --> 00:38:06,680
Speaker 1: had to be like a point. Everything had to be

754
00:38:06,800 --> 00:38:09,160
Speaker 1: inside of a little point. But you're saying that they don't.

755
00:38:09,360 --> 00:38:11,960
Speaker 1: They could. They could really be like like a fluffy

756
00:38:11,960 --> 00:38:14,719
Speaker 1: cloud of four billion sons. That's right. And another cool

757
00:38:14,800 --> 00:38:16,880
Speaker 1: thing is that any amount of matter can become a

758
00:38:16,880 --> 00:38:19,120
Speaker 1: black hole as long as you put it in the

759
00:38:19,200 --> 00:38:22,360
Speaker 1: right density. Right. You take your teaspoon of earth or

760
00:38:22,360 --> 00:38:24,279
Speaker 1: a teaspoon of water, you can make that into a

761
00:38:24,280 --> 00:38:26,520
Speaker 1: black hole if you candense it down to a small

762
00:38:26,640 --> 00:38:30,480
Speaker 1: enough area. Right, however small that event horizon has to be.

763
00:38:31,000 --> 00:38:33,799
Speaker 1: But if you have enough mass, right then then it

764
00:38:33,840 --> 00:38:37,520
Speaker 1: doesn't have to be that dense. That's the point. Right,

765
00:38:37,560 --> 00:38:39,719
Speaker 1: So you take four billion sons, you can distribute them

766
00:38:39,760 --> 00:38:42,040
Speaker 1: in a really big area and it will still be

767
00:38:42,120 --> 00:38:45,080
Speaker 1: a black hole, a really huge black hole. So I

768
00:38:45,080 --> 00:38:47,920
Speaker 1: don't recommend that if you are distributing sons around, please

769
00:38:47,960 --> 00:38:50,480
Speaker 1: be careful not to make a black hole. It's easier

770
00:38:50,520 --> 00:38:53,000
Speaker 1: than you think can be careful handling those sons. Yeah,

771
00:38:53,040 --> 00:38:55,719
Speaker 1: So the point is for huge masses, it's easier to

772
00:38:55,760 --> 00:38:57,160
Speaker 1: make a black hole because they don't have to be

773
00:38:57,239 --> 00:38:59,799
Speaker 1: as dense for small masses, like you want to turn

774
00:38:59,840 --> 00:39:02,000
Speaker 1: your teaspoon of water or tea into. A black hole

775
00:39:02,239 --> 00:39:04,439
Speaker 1: has to be really dense to become a black hole.

776
00:39:04,480 --> 00:39:07,120
Speaker 1: There is a number, right, you can calculate how small

777
00:39:07,160 --> 00:39:09,120
Speaker 1: you have to compress that into. But it has to

778
00:39:09,160 --> 00:39:12,480
Speaker 1: be really dense, all right. So then, so a super

779
00:39:12,520 --> 00:39:15,839
Speaker 1: massive black hole that's a four billion times the mass

780
00:39:15,880 --> 00:39:18,200
Speaker 1: of our Sun would actually not be that dense. It

781
00:39:18,239 --> 00:39:20,839
Speaker 1: would be about us dance as a tea spoon of water,

782
00:39:21,160 --> 00:39:23,160
Speaker 1: that's right. But if you made a black hole out

783
00:39:23,200 --> 00:39:26,120
Speaker 1: of just one sun, right, then it would be really

784
00:39:26,160 --> 00:39:28,080
Speaker 1: pretty dense. It would be about as dense as a

785
00:39:28,080 --> 00:39:32,400
Speaker 1: neutron star. Oh, I see, huh about us dance, But

786
00:39:32,400 --> 00:39:35,040
Speaker 1: but it could be denser. Well, smaller black holes in

787
00:39:35,120 --> 00:39:37,799
Speaker 1: that could be denser than neutron stars. Yes, but the

788
00:39:37,840 --> 00:39:40,800
Speaker 1: smallest black hole we've ever seen is about six times

789
00:39:40,840 --> 00:39:44,000
Speaker 1: the mass of the Sun. So in terms of actual

790
00:39:44,080 --> 00:39:47,800
Speaker 1: stuff we've we've observed in the universe, then the densest

791
00:39:47,800 --> 00:39:50,920
Speaker 1: black hole we've observed is not as dense as neutron

792
00:39:51,000 --> 00:39:55,000
Speaker 1: stars because we've never seen one smaller than six solar

793
00:39:55,040 --> 00:39:57,719
Speaker 1: masses and I have to be smaller than that to

794
00:39:57,719 --> 00:40:00,279
Speaker 1: be denser. But so why haven't we seen one? Could

795
00:40:00,280 --> 00:40:04,160
Speaker 1: one exist? They certainly could exist. Yeah, there's no minimum

796
00:40:04,239 --> 00:40:06,600
Speaker 1: size to a black hole. Remember, at the large Hadron Collider,

797
00:40:06,640 --> 00:40:08,680
Speaker 1: we think we might create black holes and those black

798
00:40:08,719 --> 00:40:12,160
Speaker 1: holes would be like particle sized, So there's no minimum

799
00:40:12,200 --> 00:40:14,520
Speaker 1: size to a black hole. So they certainly could exist.

800
00:40:14,520 --> 00:40:16,520
Speaker 1: There could be black holes out there that are the

801
00:40:16,520 --> 00:40:18,359
Speaker 1: mass of the Sun, or half the mass of the Sun,

802
00:40:18,680 --> 00:40:21,600
Speaker 1: or the mass of one Horge for example. They could exist,

803
00:40:21,880 --> 00:40:24,319
Speaker 1: but they're harder to see, right. Smaller black holes are

804
00:40:24,360 --> 00:40:26,880
Speaker 1: harder to see. So the densest thing in any of

805
00:40:26,920 --> 00:40:30,719
Speaker 1: the universe is probably a black hole, but it would

806
00:40:30,760 --> 00:40:35,760
Speaker 1: have to a be a small black hole less massive

807
00:40:35,800 --> 00:40:39,400
Speaker 1: than our sun and be we haven't seen what. So

808
00:40:39,440 --> 00:40:42,839
Speaker 1: technically the densest thing we've seen is a neutron star.

809
00:40:43,360 --> 00:40:45,760
Speaker 1: But the densest thing that could exist is a small

810
00:40:45,760 --> 00:40:48,880
Speaker 1: black hole unless you're willing to pierce the veil of

811
00:40:48,880 --> 00:40:51,919
Speaker 1: the event horizon and talk about what's going on inside

812
00:40:51,960 --> 00:40:56,080
Speaker 1: the black hole. What's inside a hole? Right, Well, then

813
00:40:56,120 --> 00:40:59,120
Speaker 1: that's the thing we don't know right now. Originally, Einstein

814
00:40:59,160 --> 00:41:01,759
Speaker 1: and general Relative they say, in the center of a

815
00:41:01,800 --> 00:41:04,600
Speaker 1: black hole is a singularity is a point, and a

816
00:41:04,680 --> 00:41:07,600
Speaker 1: singularity means a point of infinite density, right, at a

817
00:41:07,600 --> 00:41:10,120
Speaker 1: point where there is a huge amount of mass in

818
00:41:10,360 --> 00:41:13,400
Speaker 1: zero volume, which is pretty hard to get your mind around,

819
00:41:13,440 --> 00:41:15,840
Speaker 1: like how do you have stuff in no space? But

820
00:41:15,960 --> 00:41:17,960
Speaker 1: black holes are hard to get your mind around anyway,

821
00:41:18,239 --> 00:41:20,080
Speaker 1: So that's what Einstein would say. I would say, Oh,

822
00:41:20,120 --> 00:41:22,880
Speaker 1: the answer this question is obvious, it's the singularity inside

823
00:41:22,880 --> 00:41:26,719
Speaker 1: a black hole. But but que quantum mechanics, and he

824
00:41:26,719 --> 00:41:30,960
Speaker 1: wouldn't say that. His spokesperson would say that, I guess

825
00:41:31,560 --> 00:41:36,839
Speaker 1: um Foundation, that's right, the estate of Albert Einstein Um.

826
00:41:36,880 --> 00:41:39,040
Speaker 1: But the quantum mechanics folks would say, look, we know

827
00:41:39,160 --> 00:41:42,160
Speaker 1: the universe is quantum mechanical, and quantum mechanics says, you

828
00:41:42,200 --> 00:41:45,560
Speaker 1: can't have that much stuff in a well defined location, right.

829
00:41:46,040 --> 00:41:48,759
Speaker 1: Quantum mechanics says, we know there can't be a singularity

830
00:41:48,800 --> 00:41:50,640
Speaker 1: at the center of black holes. We don't know what's there,

831
00:41:50,760 --> 00:41:52,359
Speaker 1: we don't know how it works, we don't know what's

832
00:41:52,360 --> 00:41:55,560
Speaker 1: going on. And at that point gravity gets so strong

833
00:41:55,800 --> 00:41:57,759
Speaker 1: that our theories of quantum mechanics don't work, and we

834
00:41:57,800 --> 00:42:00,640
Speaker 1: don't have a theory of quantum mechanics that work when

835
00:42:00,680 --> 00:42:04,359
Speaker 1: gravity is really really powerful um, So it's a big mess.

836
00:42:04,400 --> 00:42:06,520
Speaker 1: We don't know what's going on inside a black hole.

837
00:42:06,960 --> 00:42:09,560
Speaker 1: If it's if general relativity is correct, which we're pretty

838
00:42:09,560 --> 00:42:13,120
Speaker 1: sure it's not, then there's an infinite density singularity. If

839
00:42:13,200 --> 00:42:15,880
Speaker 1: quantum mechanics is correct, which we think it is, but

840
00:42:16,000 --> 00:42:18,680
Speaker 1: it doesn't work inside a black hole, then we don't know.

841
00:42:18,840 --> 00:42:21,920
Speaker 1: So what's the densest thing in the universe? Apparently it's

842
00:42:21,960 --> 00:42:27,520
Speaker 1: the ignorance of physicists. We don't really know i'near these things.

843
00:42:28,239 --> 00:42:30,239
Speaker 1: We have no idea, that's the answer. We have no

844
00:42:30,320 --> 00:42:32,680
Speaker 1: idea what the densest thing in the universe is. It

845
00:42:32,800 --> 00:42:34,959
Speaker 1: could be a neutron star. It could be a small

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00:42:35,000 --> 00:42:37,239
Speaker 1: black hole, It could be a singularity at the center

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00:42:37,280 --> 00:42:39,360
Speaker 1: of a black hole. It could be something else weird

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00:42:39,360 --> 00:42:41,959
Speaker 1: and quantum mechanical that's going on inside a black hole.

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00:42:42,360 --> 00:42:44,319
Speaker 1: We just don't know, all right. So that so that's

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00:42:44,320 --> 00:42:45,840
Speaker 1: the answer to what is the dnist thing at the

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00:42:45,920 --> 00:42:48,359
Speaker 1: universe is? We don't know exactly, and it kind of

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00:42:48,400 --> 00:42:53,120
Speaker 1: depends on what we've observed and what the true theory

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00:42:53,239 --> 00:42:57,040
Speaker 1: of physics is at these extreme situations. That's right. But

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00:42:57,080 --> 00:43:00,160
Speaker 1: the densest thing we've ever found is a neutrons are,

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00:43:00,239 --> 00:43:04,680
Speaker 1: which is plenty dance to impress you about extreme densities

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00:43:04,719 --> 00:43:07,520
Speaker 1: in the universe, right, it goes from like a proton

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00:43:08,120 --> 00:43:11,000
Speaker 1: in a teaspoon up to a million Eiffel towers in

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00:43:11,040 --> 00:43:14,239
Speaker 1: the teaspoon. So there's an enormous range of densities. You know.

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00:43:14,280 --> 00:43:17,480
Speaker 1: The universe is not just like uniform and spread out right,

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00:43:17,520 --> 00:43:21,960
Speaker 1: it's like mostly empty with these incrediblely tight packed pockets.

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00:43:22,000 --> 00:43:25,360
Speaker 1: And that works even in France. That works email in France,

862
00:43:25,480 --> 00:43:28,319
Speaker 1: exactly all right. Thanks for joining us and another one

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00:43:28,360 --> 00:43:31,480
Speaker 1: of our Extreme Universe series. We hope you enjoyed that.

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00:43:31,719 --> 00:43:33,400
Speaker 1: Thanks for tuning in, and hey, if you have a

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00:43:33,480 --> 00:43:36,040
Speaker 1: question about the universe or or want us to talk

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00:43:36,080 --> 00:43:38,560
Speaker 1: about another extreme thing in the universe, let us know.

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00:43:46,400 --> 00:43:48,719
Speaker 1: If you still have a question after listening to all

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00:43:48,760 --> 00:43:51,960
Speaker 1: these explanations, please drop us a line. We'd love to

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00:43:52,000 --> 00:43:54,400
Speaker 1: hear from you. You can find us at Facebook, Twitter,

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00:43:54,520 --> 00:43:58,160
Speaker 1: and Instagram at Daniel and Jorge That's one word, or

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00:43:58,280 --> 00:44:02,520
Speaker 1: email us at Feedback Daniel and Jorge dot com. Thanks

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00:44:02,520 --> 00:44:05,160
Speaker 1: for listening and remember that Daniel and Jorge Explain the

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00:44:05,239 --> 00:44:08,359
Speaker 1: Universe is a production of I Heart Radio. For more

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00:44:08,440 --> 00:44:11,759
Speaker 1: podcast from my Heart Radio, visit the i Heart Radio app,

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00:44:12,080 --> 00:44:15,560
Speaker 1: Apple Podcasts or wherever you listen to your favorite shows,