WEBVTT - Do we live in a super bubble?

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<v Speaker 1>Think about where you are right now. Maybe you're in

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<v Speaker 1>your car commuting, or you're out walking the dogs or

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<v Speaker 1>at home doing the dishes. But where are you relative

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<v Speaker 1>to everyone else? How do you define it? Probably you

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<v Speaker 1>zoom out and put yourself in a wider context, your town,

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<v Speaker 1>your region, your whole country. Listeners to this pod will

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<v Speaker 1>likely be inclined to zoom out even further to all

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<v Speaker 1>of Earth and then the whole Solar System. From there,

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<v Speaker 1>it's very tempting to skip forward and put our solar

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<v Speaker 1>system into its place in the galaxy, than the galaxy

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<v Speaker 1>into its cluster, and then that cluster within the supercluster foam.

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<v Speaker 1>But have we been too hasty? Is our galaxy so simple,

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<v Speaker 1>just a collection of stars floating around a central black hole?

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<v Speaker 1>Or is there more nuance to our galactic context? We

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<v Speaker 1>think of the galaxy as mostly stars, but they're formed,

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<v Speaker 1>they burn, and they die. There's a constant slashing of

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<v Speaker 1>energy back and forth between those stars and vast clouds

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<v Speaker 1>of raw material. Where is our Solar system relative to

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<v Speaker 1>those clouds? Are we in the midst of a galactic fog?

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<v Speaker 1>Or are we floating through an open bubble? Today on

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<v Speaker 1>the pod will zoom out to this fascinating scene, understand

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<v Speaker 1>the dynamics of star formation and destruction, and let you

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<v Speaker 1>know exactly where you we all of us stand galactically speaking.

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<v Speaker 1>Welcome to Daniel and Kelly's Extraordinary Galaxy.

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<v Speaker 2>Hello, I'm Kelly Winer Smith. I study parasites and space

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<v Speaker 2>and I love bubbles.

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<v Speaker 1>Well, Hi, I'm Daniel. I'm a particle physicist. I love bubbles,

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<v Speaker 1>and I have all of my organs.

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<v Speaker 2>Okay, yeah, right, So that I was gonna ask you

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<v Speaker 2>about the most painful thing you ever experienced in your

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<v Speaker 2>life as a lead into why my laugh is going

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<v Speaker 2>to be a little off today, folks.

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<v Speaker 1>I'm going to try to restrain myself from being funny

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<v Speaker 1>today because if I make a joke that makes Kelly

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<v Speaker 1>crack up, she could literally crack up.

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<v Speaker 2>Oh I could, Yes, I could split a stitch. So

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<v Speaker 2>what aside from labor, The most painful thing that ever

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<v Speaker 2>happens to me was the gallstones that tried to pass

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<v Speaker 2>their way out of my body on Friday, but ended

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<v Speaker 2>up getting removed surgically. The whole thing, the whole gallbladder

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<v Speaker 2>was removed, and so I am still working on resolving

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<v Speaker 2>my stitches. And so it hurts to laugh. So I

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<v Speaker 2>think I've come up with the way to laugh that

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<v Speaker 2>it hurts less, and so my my laugh will sound

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<v Speaker 2>a little I don't know, maybe even less annoying. I

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<v Speaker 2>have seen there's a couple complaints about the way I laugh.

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<v Speaker 2>You'all can just kiss my rear ends. But anyway, Daniel,

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<v Speaker 2>what is the most painful thing that's ever happened to you?

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<v Speaker 1>Oh? Most painful thing that's ever happened to me? I

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<v Speaker 1>broken my wrist, but weirdly that didn't hurt that much.

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<v Speaker 1>I think maybe the most painful thing is when I

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<v Speaker 1>broke my little toe. I like massively stubbed it on

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<v Speaker 1>a little concrete outpost and cracked it and wow, yeah,

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<v Speaker 1>I thought I was gonna die.

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<v Speaker 2>Ouch. Yeah, And how long did it take to heal?

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<v Speaker 2>What do you do? Just put like a nothing.

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<v Speaker 1>You just tape it to the next toe, and like

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<v Speaker 1>whatever happens inside of it happens. Like there's no surgery

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<v Speaker 1>to correct, like the little bones inside your little toe,

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<v Speaker 1>nobody needs it. I was like, just cut that bugger off,

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<v Speaker 1>but I was like, no, you just tape it to

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<v Speaker 1>the next one. That's it.

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<v Speaker 2>Well, you know, Daniel, it sounds like if you lived

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<v Speaker 2>in a bubble, you would have been safe. But if

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<v Speaker 2>I lived in a bubble, well, that wouldn't have saved me.

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<v Speaker 2>And so well, you know, maybe if the whole universe

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<v Speaker 2>was in a bubble, that would save us from some

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<v Speaker 2>of the bumps and bruises of existence. But do we

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<v Speaker 2>live in a bubble? Daniel?

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<v Speaker 1>Well, we are trying to pop the bubble of ignorance

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<v Speaker 1>out there and help everybody understand their cosmic context, where

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<v Speaker 1>we are situated in our solar system, where our solar

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<v Speaker 1>system is situated in the galaxy, and the whole context

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<v Speaker 1>for our existence. I love filling in all those details

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<v Speaker 1>and helping people understand really where they live. And today

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<v Speaker 1>we're going to dive into that topic essentially, where our

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<v Speaker 1>sun is in the galaxy? Is there structure out there?

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<v Speaker 1>How does it all work?

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<v Speaker 2>And I think all of our inner kids are excited

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<v Speaker 2>today to find out whether or not we live in

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<v Speaker 2>a super bubble.

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<v Speaker 1>So before we dive into it, I was wondering what

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<v Speaker 1>people out there knew on the topic. So I went

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<v Speaker 1>to our group of volunteers, I asked them, do we

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<v Speaker 1>live in a super bubble? Here's what folks had to say,

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<v Speaker 1>I don't even really know what a super bubble is,

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<v Speaker 1>so maybe what do you think, Glen. I have no

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<v Speaker 1>idea what a super bubble is. I have not heard

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<v Speaker 1>the term super bubble. It makes me think about some

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<v Speaker 1>conceptualizations of fourth dimensionality.

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<v Speaker 3>Considering I couldn't tell you what a super bubble is.

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<v Speaker 3>I can't really say if we live in one, but

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<v Speaker 3>it sounds like one of these really exciting astrophysical maybe

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<v Speaker 3>who knows cool universe things, so I'm eager to learn

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<v Speaker 3>about it. I have never heard of the term super bubble,

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<v Speaker 3>but we probably live in one.

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<v Speaker 2>I like the I've never heard of it, so yes,

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<v Speaker 2>this is.

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<v Speaker 1>Really exciting to me that nobody had heard of it,

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<v Speaker 1>because it means we get to share this really cool

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<v Speaker 1>thing about the universe with everybody. Yay.

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<v Speaker 2>We love doing that.

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<v Speaker 1>You know that great XKCD comic. I mean they're all great,

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<v Speaker 1>but the one about the moment you discover somebody doesn't

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<v Speaker 1>know something really cool about the universe and how you

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<v Speaker 1>should treat that with reverence and respect because it's a

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<v Speaker 1>wonderful teaching moment. That's where we are today about super bubbles.

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<v Speaker 2>I mean, I think we can all agree that Randall

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<v Speaker 2>Monroe is the greatest web cartoonist to have ever lived.

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<v Speaker 1>Right, Wow, that's instant karma right there. Wow. I hope

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<v Speaker 1>Zach is listening and laughing at that.

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<v Speaker 2>All right, all right, bubbles, all.

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<v Speaker 1>Right, bubbles. So we're talking about the Sun and the

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<v Speaker 1>Solar System's context in the galaxy. But before we get there,

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<v Speaker 1>let's do like an overview of like what's out there

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<v Speaker 1>in space? How empty is it? Anyway? So to get oriented,

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<v Speaker 1>remember that our situation here on Earth is very unusual.

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<v Speaker 1>Like the density of stuff around you is very rare

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<v Speaker 1>in the universe. The universe is mostly very very low density,

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<v Speaker 1>and we live in a very very high density situation.

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<v Speaker 1>The Earth, of course, is wonderful and cozy, and in

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<v Speaker 1>like a normal atmosphere, you'll find a huge number of

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<v Speaker 1>molecules per cubic meter, like ten to the twenty five

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<v Speaker 1>molecules per cubic meter. It's a big number. And that's

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<v Speaker 1>just because like Avagadro's number is pretty big, and gravity

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<v Speaker 1>has gathered the Earth and the stars and all that

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<v Speaker 1>stuff together into little dense clumps.

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<v Speaker 2>I thought Avagadro's number was ten to the twenty three.

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<v Speaker 1>It is, yeah, exactly.

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<v Speaker 2>Oh but this is ten to the twenty fifth.

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<v Speaker 1>Yeah, because a mole is less than a cubic meter.

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<v Speaker 2>Got it, got it. I'm with you now, Okay, these

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<v Speaker 2>are big numbers, Daniel, big numbers.

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<v Speaker 1>These are big numbers. And you know, sometimes on Earth

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<v Speaker 1>we want to do experiments in low density situations, like

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<v Speaker 1>when we collide particles together, we don't want a whole

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<v Speaker 1>bunch of other particles around, Or when you build a

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<v Speaker 1>plasma inside eater to diffusion, you want mostly a vacuum

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<v Speaker 1>before you start. And so we have all these vacuums

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<v Speaker 1>in labs. We've created these situations you pump out all

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<v Speaker 1>the air, and you might be surprised to learn that

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<v Speaker 1>even in those highly specialized vacuums on Earth, we still

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<v Speaker 1>have something like ten to the twelve or ten to

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<v Speaker 1>the fifteen molecules per cubic meter. Like that's down ten

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<v Speaker 1>or thirteen orders of magnitude from your general atmosphere. So like,

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<v Speaker 1>really good work, and this is not easy, but still

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<v Speaker 1>it's a lot of molecules.

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<v Speaker 2>When somebody says the vacuum of space, are we doing

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<v Speaker 2>better than the vacuum of space? When we make a

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<v Speaker 2>vacuum in the lab or are we doing about the

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<v Speaker 2>same as the quote unquote vacuum of space.

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<v Speaker 1>Neither. We're not doing anywhere close to the vacuum of space.

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<v Speaker 1>The density of vacuums in labs here on Earth is

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<v Speaker 1>much higher, is much much more stuff in our lab

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<v Speaker 1>quote unquote vacuums than there is out there in space. Okay,

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<v Speaker 1>but let's stick into that and zoom our mental picture

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<v Speaker 1>out from the surface of the Earth. Obviously, the atmosphere

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<v Speaker 1>drops gradually, right, There's no like huge wall or gait

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<v Speaker 1>or anything. This is not space balls, where atmosphere is

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<v Speaker 1>that contained by a huge bubble right where the code

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<v Speaker 1>is one two three four. But in a funny way,

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<v Speaker 1>there is because space officially starts at like one hundred

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<v Speaker 1>kilometers above the surface of the Earth, which I always

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<v Speaker 1>thought was weird.

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<v Speaker 2>There's some debate about that though, isn't there.

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<v Speaker 1>Yes, absolutely there is, and like you can be an

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<v Speaker 1>astronaut if you've gone eighty kilometers above. There's definitely a debate.

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<v Speaker 1>It's something about astronomy, so it's not just it depends.

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<v Speaker 1>It's a bunch of nerds arguing about it.

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<v Speaker 2>I thought one hundred kilometers was something like at that point,

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<v Speaker 2>there aren't enough molecules to hold up your airplane anymore,

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<v Speaker 2>and so that's where space starts.

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<v Speaker 1>Oh that's cool, isn't it.

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<v Speaker 2>The Von Carmon line.

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<v Speaker 1>That's the Von Carmen line. Yeah, And the ISS is

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<v Speaker 1>like three hundred or four hundred kilometers above the surface

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<v Speaker 1>of the Earth, so definitely in space. And so if

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<v Speaker 1>you're inside our Solar system but outside Earth and its atmosphere,

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<v Speaker 1>then there's still stuff out there. The vacuum of space

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<v Speaker 1>inside the Solar System is not a perfect vacuum. There's

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<v Speaker 1>a bunch of particles. Most of it comes from the

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<v Speaker 1>Sun because the Sun, as we say often is producing

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<v Speaker 1>a lot of stuff, not just photons but also matter.

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<v Speaker 1>The solar wind is electronic and protons and alpha particles.

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<v Speaker 1>These things are zooming around with a lot of energy.

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<v Speaker 1>And so there's something like ten million protons per cubic

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<v Speaker 1>meter between planets. So remember on Earth it's ten to

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<v Speaker 1>the twenty five molecules per cubic meter, labs on Earth

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<v Speaker 1>is ten to the twelve. Now we're down to like

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<v Speaker 1>ten to the seven protons per cubic meter, so that's

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<v Speaker 1>down like five or six orders of magnitude compared to

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<v Speaker 1>vacuums on Earth.

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<v Speaker 2>Wow, you wouldn't want to go out there, people, but.

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<v Speaker 1>It would be a good place to do vacuum based experiments.

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<v Speaker 2>Sure.

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<v Speaker 1>Yeah, but it's still not that empty, right, Like millions

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<v Speaker 1>and millions of protons are out there. It's not something

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<v Speaker 1>you could say is empty. And when we talk about

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<v Speaker 1>vacuum in physics and theoretical physics, we mean space with

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<v Speaker 1>no extra energy, and it's a minimum energy state of space.

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<v Speaker 1>And so this interplanetary space is not approaching the theoretical

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<v Speaker 1>physics vacuum at all. Okay, And then take your mental

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<v Speaker 1>picture and zoom out from the Solar System and now

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<v Speaker 1>we're between stars. Were between our star and Alpha Centauri

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<v Speaker 1>for example. Now we're in what we call the interstellar medium,

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<v Speaker 1>the stuff between the stars. And even this is not

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<v Speaker 1>that empty, right. It turns out there's a big range

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<v Speaker 1>of densities of stuff from ten to the six molecule

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<v Speaker 1>percubic meter, which is like the density in our Solar system,

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<v Speaker 1>all the way down to ten to the four molecules

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<v Speaker 1>per cubic meter.

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<v Speaker 2>Isn't this where we thought the Ork cloud would be?

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<v Speaker 2>Or this is like when we get past the Ork Cloud.

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<v Speaker 1>Yeah, so there's a couple of different boundaries here. You

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<v Speaker 1>go out past the planets, you get to like the

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<v Speaker 1>dwarf planets, and then the Kuiper Belt objects. Beyond that,

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<v Speaker 1>there's the boundary of the heliosphere where the Sun dominates

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<v Speaker 1>and it meets the interstellar wind, the galactic wind. That's

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<v Speaker 1>a region where you're exiting the Solar System. But you're

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<v Speaker 1>right beyond that is more stuff. So the Orc Cloud

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<v Speaker 1>technically is part of the interstellar medium because it's past

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<v Speaker 1>that boundary. It's in a region where the interstellar wind

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<v Speaker 1>dominates over the Sun's wind, but it is gravitationally bound

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<v Speaker 1>to the Sun, so it's sort of like playing both

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<v Speaker 1>sides of the equation off.

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<v Speaker 2>That makes sense, it does, but it's still so overwhelmed

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<v Speaker 2>by the gas in that area that the interstellar medium

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<v Speaker 2>is ninety nine percent gas and all the rocks out

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<v Speaker 2>there are just make up one percent dust. Would that

0:12:17.880 --> 0:12:18.520
<v Speaker 2>be fair to say?

0:12:18.720 --> 0:12:20.360
<v Speaker 1>Yes, that's right, and we're going to come back to

0:12:20.400 --> 0:12:22.440
<v Speaker 1>the interstellar medium and do a deep dive into it.

0:12:22.440 --> 0:12:25.800
<v Speaker 1>Has a lot of really interesting structure, but yeah, most

0:12:25.800 --> 0:12:28.600
<v Speaker 1>of it is gas. It's ninety nine percent gas, and

0:12:28.640 --> 0:12:31.520
<v Speaker 1>then a little bit of it is rocks or comets,

0:12:31.559 --> 0:12:34.160
<v Speaker 1>like in the oricloud and dust. There's a few cosmic

0:12:34.240 --> 0:12:37.840
<v Speaker 1>rays out there, but mostly it's just gas and has

0:12:37.880 --> 0:12:40.400
<v Speaker 1>all sorts of interesting turbulence and structure that we're going

0:12:40.480 --> 0:12:43.320
<v Speaker 1>to talk about and don't forget out there. Also in

0:12:43.360 --> 0:12:46.720
<v Speaker 1>the galaxy is dark matter. We're only talking right now

0:12:46.760 --> 0:12:49.000
<v Speaker 1>about the luminous matter, the kind of stuff that's made

0:12:49.040 --> 0:12:52.120
<v Speaker 1>up of atoms, but we know that the universe is

0:12:52.160 --> 0:12:55.080
<v Speaker 1>dominated by dark matter. We know that it's spread out

0:12:55.120 --> 0:12:57.760
<v Speaker 1>throughout the galaxy, but it there's five times as much

0:12:57.800 --> 0:13:00.959
<v Speaker 1>of it as there is luminous matter, so you can't

0:13:01.000 --> 0:13:03.120
<v Speaker 1>interact with it, but it is there. And so if

0:13:03.160 --> 0:13:05.960
<v Speaker 1>you're just thinking about like the density of matter overall,

0:13:06.200 --> 0:13:08.079
<v Speaker 1>you have to also account for that dark matter.

0:13:08.520 --> 0:13:12.080
<v Speaker 2>Okay, so in the interstellar space mostly gas, little bit

0:13:12.120 --> 0:13:15.400
<v Speaker 2>of dust, you're not likely to stub your toe. But

0:13:15.559 --> 0:13:18.880
<v Speaker 2>so now we're talking about what's between the stars, But

0:13:18.920 --> 0:13:22.680
<v Speaker 2>what about what's between the galaxies and the intergalactic space.

0:13:23.120 --> 0:13:26.000
<v Speaker 1>Yeah, so now we're leaving the region we've ever probed directly,

0:13:26.080 --> 0:13:28.600
<v Speaker 1>Like we've sent probes that have left the Solar System

0:13:28.880 --> 0:13:32.120
<v Speaker 1>just barely like Voyager one reached the interstellar medium in

0:13:32.160 --> 0:13:35.960
<v Speaker 1>twenty twelve, Voyager two and twenty eighteen. But now we're

0:13:36.040 --> 0:13:39.000
<v Speaker 1>going well beyond where we've ever probed directly, and we're

0:13:39.040 --> 0:13:42.480
<v Speaker 1>relying just on observations and theory and stimulation. So now

0:13:42.520 --> 0:13:45.400
<v Speaker 1>between the galaxies, what is there, Well, this is something

0:13:45.400 --> 0:13:49.200
<v Speaker 1>we call very creatively the intergalactic medium, and this is

0:13:49.320 --> 0:13:53.800
<v Speaker 1>mostly rarefied plasma, so that means essentially ionized hydrogen is

0:13:53.880 --> 0:13:57.560
<v Speaker 1>just protons and out there. On average it's like one

0:13:57.640 --> 0:14:01.400
<v Speaker 1>to ten atoms per cubic meter, so a pretty small number,

0:14:01.600 --> 0:14:05.200
<v Speaker 1>but still not that small. I mean, intergalactic space is

0:14:05.559 --> 0:14:09.560
<v Speaker 1>unimaginably vast. There's just so much of it. Even if

0:14:09.600 --> 0:14:12.240
<v Speaker 1>you think about space between the planets as being big,

0:14:12.520 --> 0:14:14.760
<v Speaker 1>and most of the space and the Solar System is

0:14:14.800 --> 0:14:17.920
<v Speaker 1>the space between the planets, right, planets and the Sun

0:14:18.040 --> 0:14:21.040
<v Speaker 1>are rare, like you're randomly sampled inside the Solar System.

0:14:21.080 --> 0:14:22.960
<v Speaker 1>You would very rarely touch a planet or a star

0:14:23.640 --> 0:14:27.080
<v Speaker 1>inside the galaxy. Right structure is also very rare. But

0:14:27.120 --> 0:14:29.960
<v Speaker 1>between the galaxies, it's even hard to comprehend because we

0:14:30.000 --> 0:14:33.360
<v Speaker 1>have like millions of light years between these galaxies, and

0:14:33.480 --> 0:14:36.280
<v Speaker 1>yet it's still filled with stuff. There's one to ten

0:14:36.320 --> 0:14:40.760
<v Speaker 1>atoms out there, and actually these tendrils of plasma there's

0:14:40.800 --> 0:14:43.800
<v Speaker 1>also structure to it. It's not just randomly distributed. All

0:14:43.840 --> 0:14:47.360
<v Speaker 1>the galaxies are connected by these tendrils of plasma, these filaments,

0:14:47.920 --> 0:14:50.480
<v Speaker 1>and something like half of all the atoms in the

0:14:50.560 --> 0:14:54.720
<v Speaker 1>universe are outside of galaxies and are inside these tendrils

0:14:54.800 --> 0:14:55.960
<v Speaker 1>between galaxies.

0:14:56.000 --> 0:14:58.120
<v Speaker 2>It's incredible, wow, And how do they get there? Do

0:14:58.320 --> 0:15:00.400
<v Speaker 2>they get like shot out by suns? They were just

0:15:00.440 --> 0:15:02.800
<v Speaker 2>there from the beginning of the creation of the universe

0:15:02.840 --> 0:15:03.840
<v Speaker 2>and they just stayed.

0:15:03.520 --> 0:15:07.080
<v Speaker 1>There both and all of those like there's a feedback

0:15:07.120 --> 0:15:12.040
<v Speaker 1>loop where galaxies are emitting particles right, supernovas and shockwaves

0:15:12.080 --> 0:15:15.640
<v Speaker 1>and all sorts of stuff. But mostly this structure represents

0:15:15.840 --> 0:15:19.480
<v Speaker 1>the dark matter structure of the universe. Galaxies form in

0:15:19.480 --> 0:15:22.000
<v Speaker 1>the deepest wells and then there are tendrils of dark

0:15:22.040 --> 0:15:24.960
<v Speaker 1>matter between these wells, and that's where you find these

0:15:24.960 --> 0:15:27.760
<v Speaker 1>tendrils of plasma. So the plasma is like a tracer

0:15:27.800 --> 0:15:30.760
<v Speaker 1>that tells you where the dark matter is. And also

0:15:30.880 --> 0:15:33.440
<v Speaker 1>between these galaxies, of course, is a significant amount of

0:15:33.520 --> 0:15:36.200
<v Speaker 1>dark energy. Dark energy is everywhere in space. It's just

0:15:36.240 --> 0:15:39.640
<v Speaker 1>a really, really tiny amount, but because it doesn't get diluted,

0:15:39.640 --> 0:15:43.320
<v Speaker 1>as the universe expands over vast spaces, it really starts

0:15:43.320 --> 0:15:45.840
<v Speaker 1>to add up. Between the galaxies, you have to start

0:15:45.880 --> 0:15:48.840
<v Speaker 1>accounting for the dark energy. And then as you zoom out,

0:15:48.960 --> 0:15:53.160
<v Speaker 1>galaxies form clusters, and between those clusters most of the

0:15:53.280 --> 0:15:56.120
<v Speaker 1>energy density between those clusters. It's not matter at all.

0:15:56.360 --> 0:15:59.440
<v Speaker 1>It's dark energy, all right.

0:15:59.560 --> 0:16:02.920
<v Speaker 2>So at the big scale, we're mostly thinking about dark energy,

0:16:03.080 --> 0:16:06.200
<v Speaker 2>and as we zoom in, we're starting to think about gas.

0:16:07.920 --> 0:16:10.200
<v Speaker 2>Let's take a break, and when we come back, I

0:16:10.240 --> 0:16:13.600
<v Speaker 2>want to go back to the interstellar medium and go

0:16:13.640 --> 0:16:36.320
<v Speaker 2>into more detail about what's there. Yeah, and we're back,

0:16:36.360 --> 0:16:38.440
<v Speaker 2>and Daniel is going to be telling us more about

0:16:38.440 --> 0:16:40.800
<v Speaker 2>what is in the interstellar medium.

0:16:40.840 --> 0:16:43.200
<v Speaker 1>That's right. Today we're talking about the context of our

0:16:43.240 --> 0:16:45.320
<v Speaker 1>solar system where it is and how much stuff there

0:16:45.400 --> 0:16:48.800
<v Speaker 1>is around us, and whether our solar system is jumping

0:16:48.920 --> 0:16:52.840
<v Speaker 1>into a huge bubble in the galaxy. Sounds fun, and

0:16:52.880 --> 0:16:55.320
<v Speaker 1>so the important thing is to understand this bit between

0:16:55.400 --> 0:16:57.680
<v Speaker 1>the stars. And the thing I love doing is going

0:16:57.720 --> 0:17:01.080
<v Speaker 1>back in history and understanding when we understood something and

0:17:01.080 --> 0:17:04.680
<v Speaker 1>what our early silly ideas were, you know, because it's

0:17:04.680 --> 0:17:07.000
<v Speaker 1>easy to just like, download all of human knowledge into

0:17:07.040 --> 0:17:10.320
<v Speaker 1>your brain right now. But remember that people like struggled

0:17:10.359 --> 0:17:12.439
<v Speaker 1>and puzzled to figure this out, and there were many

0:17:12.520 --> 0:17:16.320
<v Speaker 1>wrong paths and silly ideas entertained for hundreds of years

0:17:16.359 --> 0:17:17.120
<v Speaker 1>along the way.

0:17:17.480 --> 0:17:19.639
<v Speaker 2>It's kind of cute to imagine that nobody in like

0:17:19.680 --> 0:17:21.320
<v Speaker 2>fifty years is going to look back at us and

0:17:21.359 --> 0:17:24.639
<v Speaker 2>be like, oh, remember that cute thing that the physicists

0:17:24.640 --> 0:17:28.320
<v Speaker 2>thought in twenty twenty six about anyway, they could be

0:17:28.400 --> 0:17:30.840
<v Speaker 2>laughing at us eventually, but let's go ahead and laugh

0:17:30.880 --> 0:17:31.200
<v Speaker 2>at them.

0:17:33.040 --> 0:17:37.160
<v Speaker 1>So first, remember, in the broader context, we didn't know

0:17:37.240 --> 0:17:41.199
<v Speaker 1>that our galaxy was one of many galaxies until like

0:17:41.240 --> 0:17:44.200
<v Speaker 1>the early nineteen hundreds, right, we thought we had a galaxy.

0:17:44.400 --> 0:17:46.359
<v Speaker 1>It was a bunch of stars and that was it.

0:17:46.359 --> 0:17:48.800
<v Speaker 1>It was just our galaxy, and that was everything. The

0:17:48.840 --> 0:17:52.280
<v Speaker 1>galaxy was basically the universe and everything that was out

0:17:52.320 --> 0:17:54.840
<v Speaker 1>there that wasn't actually in our galaxy, but we didn't

0:17:54.840 --> 0:17:56.760
<v Speaker 1>know it yet. We called like a nebula because it

0:17:56.840 --> 0:17:59.440
<v Speaker 1>was like a smeary blob in the sky we couldn't resolve.

0:18:00.160 --> 0:18:02.160
<v Speaker 1>So that's sort of like the bigger picture. But then

0:18:02.200 --> 0:18:04.560
<v Speaker 1>what about inside the galaxy, Well, people try to make

0:18:04.640 --> 0:18:07.119
<v Speaker 1>like maps of the galaxy early on to try to

0:18:07.200 --> 0:18:10.240
<v Speaker 1>understand the structure. But we're interested in like the bit

0:18:10.359 --> 0:18:13.280
<v Speaker 1>between the stars. And it was like the late seventeen

0:18:13.320 --> 0:18:16.280
<v Speaker 1>hundreds people started to wonder, like, hmm, is the space

0:18:16.359 --> 0:18:20.440
<v Speaker 1>between the stars really a vacuum or is there something there?

0:18:21.119 --> 0:18:24.200
<v Speaker 1>You know? And how would we know? And this coincides

0:18:24.200 --> 0:18:27.960
<v Speaker 1>a little bit later with Maxwell's development of electromagnetism, the

0:18:28.040 --> 0:18:32.200
<v Speaker 1>idea that light is a balance between electricity and magnetism.

0:18:32.400 --> 0:18:35.160
<v Speaker 1>The energy slashes back and forth between the two fields,

0:18:35.400 --> 0:18:38.440
<v Speaker 1>but then it moves as a wave in these fields

0:18:38.800 --> 0:18:41.080
<v Speaker 1>at the speed of light. And this is Maxwell's great

0:18:41.080 --> 0:18:44.280
<v Speaker 1>discovery that light is a wave, which of course begged

0:18:44.280 --> 0:18:47.879
<v Speaker 1>the question of a wave in what right, And so

0:18:48.119 --> 0:18:52.040
<v Speaker 1>we saw the rise of the theory of the luminiferous ether. Right.

0:18:52.160 --> 0:18:55.000
<v Speaker 1>This is a famous theory which was invented to explain

0:18:55.800 --> 0:18:59.080
<v Speaker 1>what light is wiggling? Right, Maybe there's something out there,

0:18:59.119 --> 0:19:02.600
<v Speaker 1>like if waves are wiggles and water, and sounds wiggles

0:19:02.600 --> 0:19:05.200
<v Speaker 1>and air, maybe light is a wiggle in this luminiferous

0:19:05.200 --> 0:19:08.560
<v Speaker 1>ether that we hadn't ever discovered before it fills the universe.

0:19:09.040 --> 0:19:12.879
<v Speaker 1>So this would be an early theory of the interstellar medium.

0:19:12.920 --> 0:19:15.240
<v Speaker 1>What is out there between the stars, what allows the

0:19:15.320 --> 0:19:18.080
<v Speaker 1>light to go from Alpha Centauri to us here?

0:19:18.600 --> 0:19:21.600
<v Speaker 2>And so the luminiferous ether. I thought I was going

0:19:21.680 --> 0:19:24.320
<v Speaker 2>to get it on the first shot. Totally did I

0:19:24.400 --> 0:19:28.320
<v Speaker 2>stumbled a little. Would you find that between like Earth

0:19:28.520 --> 0:19:31.800
<v Speaker 2>and Mars or that was just between the end of

0:19:31.840 --> 0:19:34.640
<v Speaker 2>our solar system and the start of the next solar system?

0:19:35.000 --> 0:19:37.760
<v Speaker 1>Great question. No, is should be everywhere. If it exists,

0:19:37.800 --> 0:19:40.720
<v Speaker 1>it should be everywhere. And that was key because people

0:19:40.760 --> 0:19:42.159
<v Speaker 1>looked for it and they said, well, let's try to

0:19:42.200 --> 0:19:46.160
<v Speaker 1>measure our velocity through this ether. If it's out there

0:19:46.200 --> 0:19:48.680
<v Speaker 1>and it's a medium for light, light is wiggling through

0:19:48.680 --> 0:19:52.080
<v Speaker 1>this ether, then Earth moving around the Sun should be

0:19:52.200 --> 0:19:56.000
<v Speaker 1>moving zigzagging basically back and forth through this ether. And

0:19:56.080 --> 0:19:58.720
<v Speaker 1>if light has a constant velocity relative to the ether,

0:19:59.240 --> 0:20:01.200
<v Speaker 1>then we should be able to measure light moving in

0:20:01.280 --> 0:20:05.080
<v Speaker 1>different velocities as we move in different velocities through the ether. Okay, right,

0:20:05.119 --> 0:20:07.399
<v Speaker 1>the same way that like you can catch up to

0:20:07.520 --> 0:20:10.040
<v Speaker 1>sound waves and air because they have a constant velocity

0:20:10.119 --> 0:20:12.399
<v Speaker 1>relative to the air, so you can catch up to

0:20:12.440 --> 0:20:14.800
<v Speaker 1>them and even pass them. Right, just like when you're

0:20:14.800 --> 0:20:16.840
<v Speaker 1>on a boat in a lake, you're making ripples. If

0:20:16.880 --> 0:20:18.719
<v Speaker 1>you go fast enough, you can catch up to them,

0:20:18.760 --> 0:20:22.320
<v Speaker 1>which it gives you awake, right, And so if light

0:20:22.400 --> 0:20:24.160
<v Speaker 1>is moving through this ether, and then as the Earth

0:20:24.200 --> 0:20:26.320
<v Speaker 1>moves around the Sun, we should see a change in

0:20:26.359 --> 0:20:29.520
<v Speaker 1>the velocity of light famous Michaelson. More the experiment of

0:20:29.520 --> 0:20:32.639
<v Speaker 1>course proved that light is the same speed year round,

0:20:32.720 --> 0:20:36.119
<v Speaker 1>regardless of the direction, and so apparently there is no

0:20:36.280 --> 0:20:39.320
<v Speaker 1>luminiferous ether. So then people are like, oh, wow, maybe

0:20:39.440 --> 0:20:41.880
<v Speaker 1>there really is a vacuum in between the stars.

0:20:42.119 --> 0:20:44.240
<v Speaker 2>And you all didn't find another use for the word

0:20:44.480 --> 0:20:47.440
<v Speaker 2>luminiferous ether. That's a total bummer because it just sounds

0:20:47.520 --> 0:20:49.920
<v Speaker 2>so nice.

0:20:50.400 --> 0:20:53.760
<v Speaker 1>Well, these days is actually a proliferation of ether theories,

0:20:54.000 --> 0:20:57.280
<v Speaker 1>which is very confusing because ether most generally just refers

0:20:57.320 --> 0:21:00.520
<v Speaker 1>to like a theory of the substrate of space, and

0:21:00.600 --> 0:21:03.480
<v Speaker 1>our current theory that quantum field theory, where space is

0:21:03.480 --> 0:21:07.080
<v Speaker 1>filled with these fields and these fields exist in space.

0:21:07.400 --> 0:21:10.560
<v Speaker 1>Then that's sort of the modern ether, and that's totally

0:21:10.600 --> 0:21:13.560
<v Speaker 1>cool and nobody objects to that. But that's an ether

0:21:13.640 --> 0:21:17.399
<v Speaker 1>where you can't measure your velocity relative to it, like

0:21:17.520 --> 0:21:20.320
<v Speaker 1>the luminiferous ether has a frame it's at rest in

0:21:20.359 --> 0:21:23.399
<v Speaker 1>some frame, and light moves at a constant speed only

0:21:23.440 --> 0:21:27.600
<v Speaker 1>in that frame. The modern ether quantum field theory vacuum

0:21:28.000 --> 0:21:31.160
<v Speaker 1>has no frame. And so there's a big distinction between

0:21:31.200 --> 0:21:35.080
<v Speaker 1>the luminiferous ether of two centuries ago and today's concepts

0:21:35.080 --> 0:21:37.840
<v Speaker 1>of the ether. And in lots of pop side descriptions

0:21:37.880 --> 0:21:41.920
<v Speaker 1>you see this important distinction sort of ignored or fuzzed over.

0:21:42.440 --> 0:21:45.040
<v Speaker 2>Okay, all right, and I could use a quick step

0:21:45.080 --> 0:21:46.920
<v Speaker 2>back and a reminder about where we are. So we've

0:21:46.960 --> 0:21:51.320
<v Speaker 2>been talking about what is in space between things. Yeah,

0:21:51.359 --> 0:21:53.920
<v Speaker 2>and we've just established that we used to think there

0:21:54.000 --> 0:21:57.119
<v Speaker 2>was ether between stuff, but there's not. But there's not,

0:21:57.280 --> 0:22:00.160
<v Speaker 2>but there's not. And so now, okay, so we're going

0:22:00.160 --> 0:22:02.560
<v Speaker 2>through the history of our understanding of what was in

0:22:02.600 --> 0:22:04.000
<v Speaker 2>the interstellar medium.

0:22:04.480 --> 0:22:07.760
<v Speaker 1>That's right. And then in eighteen ninety nine people discovered, oh,

0:22:07.760 --> 0:22:10.400
<v Speaker 1>there is some actual stuff out there between the stars,

0:22:10.760 --> 0:22:13.919
<v Speaker 1>not ether, but like actual matter. There were these things

0:22:13.960 --> 0:22:17.680
<v Speaker 1>called dark nebulae, essentially these dusty clouds you could see

0:22:17.720 --> 0:22:21.760
<v Speaker 1>out there that passed between the stars, right between us

0:22:21.800 --> 0:22:24.240
<v Speaker 1>and other stars. There were like these clouds of stuff

0:22:24.640 --> 0:22:28.439
<v Speaker 1>which were sometimes silhouetted against this background starfield. This is

0:22:28.520 --> 0:22:32.680
<v Speaker 1>essentially the first discovery of interstellar gas. It's just blobs

0:22:32.680 --> 0:22:35.280
<v Speaker 1>of gas that are out there between the stars. And

0:22:35.320 --> 0:22:38.520
<v Speaker 1>so as you make more and more accurate observations of

0:22:38.560 --> 0:22:41.120
<v Speaker 1>these stars and understand like why they dim or what

0:22:41.160 --> 0:22:43.520
<v Speaker 1>you can see and what's between you and those stars,

0:22:43.560 --> 0:22:46.040
<v Speaker 1>you start to build a map of the galaxy and

0:22:46.119 --> 0:22:49.480
<v Speaker 1>understand like where there's dust and where there's gas. And

0:22:49.520 --> 0:22:52.800
<v Speaker 1>this is our first like understanding really of the context

0:22:52.840 --> 0:22:53.720
<v Speaker 1>of our Solar.

0:22:53.400 --> 0:22:56.960
<v Speaker 2>System, understanding that there's gas out there. That gas isn't

0:22:58.000 --> 0:23:01.600
<v Speaker 2>like the ort cloud. That's just under standing where other

0:23:02.400 --> 0:23:04.560
<v Speaker 2>galaxies are out there and you're just kind of seeing

0:23:04.560 --> 0:23:06.800
<v Speaker 2>them as gas or what is that gas exactly?

0:23:07.119 --> 0:23:09.720
<v Speaker 1>Yeah, this is gas within our galaxy, okay, right, not

0:23:09.800 --> 0:23:13.560
<v Speaker 1>between galaxies. This is just understanding like what's between the stars.

0:23:13.640 --> 0:23:16.639
<v Speaker 1>Are the stars dots in a true vacuum or is

0:23:16.680 --> 0:23:18.800
<v Speaker 1>there like a soup out there? And it turns out

0:23:18.840 --> 0:23:22.480
<v Speaker 1>it's pretty soupy. We discovered these dark clouds of gas

0:23:22.520 --> 0:23:25.399
<v Speaker 1>between the stars, and then in the early nineteen hundreds

0:23:25.400 --> 0:23:29.159
<v Speaker 1>we discovered cosmic rays, which are just particles from space

0:23:29.240 --> 0:23:31.679
<v Speaker 1>that are zipping towards the Earth. And if there are

0:23:31.680 --> 0:23:34.439
<v Speaker 1>particles zpping towards the Earth. There's zipping from somewhere right,

0:23:34.440 --> 0:23:36.840
<v Speaker 1>which means that like space out there is filled with

0:23:36.880 --> 0:23:39.879
<v Speaker 1>all of these particles. So we had this growing awareness

0:23:39.880 --> 0:23:42.160
<v Speaker 1>that the space between the stars is filled with gas

0:23:42.280 --> 0:23:45.720
<v Speaker 1>and with ions and with electrons, just like in the

0:23:45.720 --> 0:23:47.800
<v Speaker 1>Solar System. And so instead of thinking of it like

0:23:48.240 --> 0:23:50.879
<v Speaker 1>here's a pocket of stuff the star and the planets,

0:23:51.720 --> 0:23:53.720
<v Speaker 1>you know how, now we think about like a spectrum

0:23:53.760 --> 0:23:56.480
<v Speaker 1>of stuff inside the Solar System, little bits of dust

0:23:56.560 --> 0:23:58.359
<v Speaker 1>all the way up to Jupiter and then the Sun.

0:23:58.800 --> 0:24:00.680
<v Speaker 1>In the same way, you should think about a smooth

0:24:00.840 --> 0:24:04.960
<v Speaker 1>transition between the Solar System and the interstellar medium that

0:24:05.040 --> 0:24:07.840
<v Speaker 1>between the stars there is still stuff. Yes, there is

0:24:07.880 --> 0:24:10.919
<v Speaker 1>a boundary where the solar wind stops dominating and the

0:24:11.000 --> 0:24:14.320
<v Speaker 1>interstellar wind starts dominating, But in terms of the distribution

0:24:14.359 --> 0:24:17.520
<v Speaker 1>of stuff, it's pretty smooth, and so you should expect

0:24:17.520 --> 0:24:19.840
<v Speaker 1>there to be stuff out there in the interstellar medium,

0:24:19.880 --> 0:24:22.160
<v Speaker 1>and it actually makes up like between ten and fifteen

0:24:22.200 --> 0:24:25.040
<v Speaker 1>percent of the mass of the galaxy is not inside

0:24:25.040 --> 0:24:28.760
<v Speaker 1>the stars. Yeah, it's between the stars, and it's going

0:24:28.840 --> 0:24:31.320
<v Speaker 1>to play an important role in how those stars are

0:24:31.359 --> 0:24:34.639
<v Speaker 1>formed and the health of our galaxy in forming stars,

0:24:34.680 --> 0:24:37.160
<v Speaker 1>whether our galaxy keeps making stars or whether it gets

0:24:37.280 --> 0:24:42.840
<v Speaker 1>quenched as they say, don't get quenched. So let's dig

0:24:43.000 --> 0:24:45.800
<v Speaker 1>a little bit more deeply into what's in the interstellar medium.

0:24:46.160 --> 0:24:48.080
<v Speaker 1>We said before the break that it's mostly gas, which

0:24:48.119 --> 0:24:51.040
<v Speaker 1>means that it's mostly hydrogen. It's like ninety percent hydrogen

0:24:51.520 --> 0:24:55.000
<v Speaker 1>ten percent helium, and the universe is mostly hydrogen, so

0:24:55.080 --> 0:24:58.280
<v Speaker 1>that makes sense. Something that's interesting, though, is that even

0:24:58.320 --> 0:25:00.760
<v Speaker 1>though there's a lot of space out there, it's super dense,

0:25:00.800 --> 0:25:03.919
<v Speaker 1>this stuff still behaves like a gas, like it interacts

0:25:03.920 --> 0:25:07.640
<v Speaker 1>with itself. It's not like non interacting, like the way

0:25:07.680 --> 0:25:09.800
<v Speaker 1>the exosphere of the Moon is just a bunch of

0:25:09.800 --> 0:25:13.040
<v Speaker 1>particles that ignore each other. Out there, these particles are

0:25:13.119 --> 0:25:16.360
<v Speaker 1>moving so fast the mean free path is pretty short,

0:25:16.680 --> 0:25:19.000
<v Speaker 1>Like they don't go very far before they run into

0:25:19.000 --> 0:25:21.520
<v Speaker 1>another one or interact with another one. They don't have

0:25:21.520 --> 0:25:24.439
<v Speaker 1>to actually touch because they have charges. They can interact

0:25:24.480 --> 0:25:26.879
<v Speaker 1>without touching each other. So that's really fast and that

0:25:26.960 --> 0:25:28.159
<v Speaker 1>was a little bit of a surprise to me when

0:25:28.200 --> 0:25:28.919
<v Speaker 1>I learned about that.

0:25:29.280 --> 0:25:32.200
<v Speaker 2>So if somebody were living out there, could they be

0:25:32.359 --> 0:25:35.360
<v Speaker 2>getting power from that, They.

0:25:35.320 --> 0:25:38.200
<v Speaker 1>Could be getting killed from that. I mean, this is radiation, right,

0:25:38.600 --> 0:25:41.480
<v Speaker 1>These particles are moving at high speeds even though it's

0:25:41.480 --> 0:25:44.600
<v Speaker 1>fairly low density. These things are moving pretty fast, like

0:25:44.920 --> 0:25:47.760
<v Speaker 1>inside the solar system, the solar wind is moving at

0:25:47.800 --> 0:25:51.359
<v Speaker 1>four hundred kilometers per second. Sometimes these particles of energy

0:25:51.400 --> 0:25:54.880
<v Speaker 1>up to ten keV, And in the interstellar medium, these

0:25:54.880 --> 0:25:58.119
<v Speaker 1>things are even higher speeds. So technically the temperature can

0:25:58.160 --> 0:26:01.080
<v Speaker 1>sometimes be like up in the millions of even though

0:26:01.080 --> 0:26:03.760
<v Speaker 1>the density is very very low, So you would like

0:26:03.880 --> 0:26:06.119
<v Speaker 1>freeze because there's not a lot of heat being deposited,

0:26:06.320 --> 0:26:08.720
<v Speaker 1>but also you'd be riddled with all of these tiny,

0:26:08.800 --> 0:26:09.800
<v Speaker 1>little high speed bullets.

0:26:09.960 --> 0:26:11.600
<v Speaker 2>That's definitely worse than New Jersey.

0:26:13.160 --> 0:26:14.639
<v Speaker 1>It's a close call, but I agree with you.

0:26:14.800 --> 0:26:17.119
<v Speaker 2>Ah, I do like New Jersey though I was born there.

0:26:17.440 --> 0:26:20.520
<v Speaker 1>The others fascinating bit about the interstellar medium is what's

0:26:20.560 --> 0:26:23.639
<v Speaker 1>not gas, which is the dust. And dust sounds like,

0:26:23.720 --> 0:26:26.040
<v Speaker 1>you know, stuff you'd sweep up and throw away, but

0:26:26.119 --> 0:26:30.080
<v Speaker 1>dust is actually super fascinating from a cosmic sense because

0:26:30.200 --> 0:26:32.800
<v Speaker 1>dust comes from dead stars. Right, Like, how do you

0:26:32.920 --> 0:26:35.919
<v Speaker 1>make dust? You need heavier elements. You need those elements

0:26:35.960 --> 0:26:38.679
<v Speaker 1>to stick together, You need them to form these little

0:26:38.720 --> 0:26:42.040
<v Speaker 1>crystals and to gather more bits to themselves, and dust

0:26:42.119 --> 0:26:46.240
<v Speaker 1>is like the seed for new solar systems and new planets. Right,

0:26:46.520 --> 0:26:49.119
<v Speaker 1>our Earth formed by a bunch of dust which bounced

0:26:49.119 --> 0:26:51.560
<v Speaker 1>into itself and stuck together and formed a bigger piece

0:26:51.560 --> 0:26:54.280
<v Speaker 1>of dust and gathered more together. So these are really

0:26:54.280 --> 0:26:56.679
<v Speaker 1>the seeds of future solar systems as well as the

0:26:56.720 --> 0:26:58.080
<v Speaker 1>ashes of previous ones.

0:26:58.480 --> 0:27:00.280
<v Speaker 2>Oh man, at first I thought you were talking about

0:27:00.280 --> 0:27:03.320
<v Speaker 2>gallstone formation, and then it sounded much more beautiful, and

0:27:03.359 --> 0:27:05.960
<v Speaker 2>I'm glad my gallstones, you know, stopped getting bigger before

0:27:06.000 --> 0:27:07.840
<v Speaker 2>they formed planets and universes.

0:27:10.440 --> 0:27:13.600
<v Speaker 1>But these huge amounts of like iron in silicon, magnesium,

0:27:14.119 --> 0:27:17.040
<v Speaker 1>a bunch of oxygen and carbon. This even like nano

0:27:17.119 --> 0:27:21.800
<v Speaker 1>diamonds and fullerines out there. They're really fascinating. And some

0:27:21.880 --> 0:27:26.000
<v Speaker 1>of these things are presolar grains, which are preserved from

0:27:26.040 --> 0:27:29.520
<v Speaker 1>the original star. So things formed like in the atmosphere

0:27:29.560 --> 0:27:31.920
<v Speaker 1>of the star, and then there's a supernova that blasts

0:27:31.920 --> 0:27:34.480
<v Speaker 1>out and spreads all these dust grains, and some of

0:27:34.520 --> 0:27:37.440
<v Speaker 1>them survive, right, They're not shattered. A lot of this

0:27:37.480 --> 0:27:41.159
<v Speaker 1>stuff is smashed into itself and shattered and reprocessed, but

0:27:41.280 --> 0:27:44.040
<v Speaker 1>some of these presolar grains survive and we actually find them,

0:27:44.080 --> 0:27:47.560
<v Speaker 1>like on the ocean floor, we can find little grains

0:27:47.560 --> 0:27:51.159
<v Speaker 1>of dust that survived a supernova and zoomed across the

0:27:51.240 --> 0:27:54.240
<v Speaker 1>universe and gathered together to help form the Earth.

0:27:54.600 --> 0:27:56.760
<v Speaker 2>How could you know? How could you find a grain

0:27:56.840 --> 0:28:01.200
<v Speaker 2>of sand and be like, I know where you came from.

0:28:01.400 --> 0:28:04.800
<v Speaker 1>Yeah, they have really unusual isotope mixtures which you only

0:28:04.880 --> 0:28:07.679
<v Speaker 1>find like in those conditions that are formed, like in

0:28:07.720 --> 0:28:09.960
<v Speaker 1>the atmospheres of supernovas. It's really incredible.

0:28:10.080 --> 0:28:11.600
<v Speaker 2>Wow, that is incredible.

0:28:12.119 --> 0:28:14.840
<v Speaker 1>And so the interstellar medium, it's mostly gas. There's a

0:28:14.880 --> 0:28:16.600
<v Speaker 1>little bit of dust out there, it's like one percent,

0:28:16.640 --> 0:28:18.600
<v Speaker 1>but I think that's the most interesting part. And then

0:28:18.640 --> 0:28:21.200
<v Speaker 1>of course some of it is very very high energy

0:28:21.200 --> 0:28:24.880
<v Speaker 1>particles zooming through space cosmic rays, and so you mix

0:28:24.920 --> 0:28:28.160
<v Speaker 1>all this together and that's what interstellar medium is made

0:28:28.160 --> 0:28:32.600
<v Speaker 1>out of. Mostly gas, which is actually mostly molecular not ionized,

0:28:32.960 --> 0:28:35.200
<v Speaker 1>and then one percent dust and then a few very

0:28:35.280 --> 0:28:36.440
<v Speaker 1>high energy ions.

0:28:36.840 --> 0:28:39.160
<v Speaker 2>All Right, we are getting closer to talking about the

0:28:39.240 --> 0:28:42.360
<v Speaker 2>amazing and exciting superbubble. So we're going to take a break,

0:28:42.480 --> 0:28:44.160
<v Speaker 2>and when we get back, we're going to talk about

0:28:44.240 --> 0:28:47.160
<v Speaker 2>how the gas and the dust are structured inside of

0:28:47.200 --> 0:29:09.720
<v Speaker 2>the interstellar medium. We are back and we're talking about

0:29:09.720 --> 0:29:12.880
<v Speaker 2>the interstellar medium, the space between the stars, and we've

0:29:13.080 --> 0:29:17.960
<v Speaker 2>established that it's mostly gas some dust in there. How

0:29:18.040 --> 0:29:20.400
<v Speaker 2>is all of that stuff structured in this space?

0:29:20.520 --> 0:29:23.160
<v Speaker 1>Daniel, Yeah, So you might imagine, oh, it's just smooth,

0:29:23.280 --> 0:29:26.280
<v Speaker 1>it's just spread out out there. But it's like a

0:29:26.360 --> 0:29:29.400
<v Speaker 1>vast fluid, which means that it has all sorts of stuff

0:29:29.440 --> 0:29:32.320
<v Speaker 1>going on. It's like our atmosphere, right, which we model

0:29:32.360 --> 0:29:35.760
<v Speaker 1>and has currents and winds and high density regions and

0:29:35.760 --> 0:29:38.960
<v Speaker 1>low density regions, and so you can think about the

0:29:39.000 --> 0:29:42.160
<v Speaker 1>interstellar medium as a vast fluid because it is interacting. Right,

0:29:42.200 --> 0:29:45.080
<v Speaker 1>The meanfree path of these particles is pretty short, but

0:29:45.120 --> 0:29:48.520
<v Speaker 1>it's also more complex than a simple fluid because often

0:29:48.520 --> 0:29:51.120
<v Speaker 1>these particles are moving really really fast. Our whole regions

0:29:51.160 --> 0:29:53.800
<v Speaker 1>of particles are moving super duper fast. So you can

0:29:53.880 --> 0:29:59.160
<v Speaker 1>have supersonic regions of this interstellar medium right places where

0:29:59.160 --> 0:30:01.480
<v Speaker 1>the gas is moved being faster than the speed of

0:30:01.560 --> 0:30:04.440
<v Speaker 1>sound in that medium. Remember, you can define the speed

0:30:04.480 --> 0:30:08.080
<v Speaker 1>of sound in anything, in water and air and steel,

0:30:08.400 --> 0:30:10.280
<v Speaker 1>and it depends like on the density of the thing.

0:30:10.680 --> 0:30:13.520
<v Speaker 1>Things that are denser, the bonds are tighter, and if

0:30:13.520 --> 0:30:16.880
<v Speaker 1>you push on one, then the pressure wave propagates more quickly,

0:30:17.200 --> 0:30:19.720
<v Speaker 1>and then it would if something was really low density,

0:30:19.840 --> 0:30:21.920
<v Speaker 1>because then the particles have to drift longer before they

0:30:21.920 --> 0:30:24.880
<v Speaker 1>bump into each other. Okay, And so what happens in

0:30:24.920 --> 0:30:28.880
<v Speaker 1>the interstellar medium is you have these shockwaves, these supersonic

0:30:28.920 --> 0:30:32.760
<v Speaker 1>shockwaves which smash into something else, and so you get

0:30:32.800 --> 0:30:35.959
<v Speaker 1>this supersonic shockwave, but that compresses the gas, makes it

0:30:36.040 --> 0:30:39.800
<v Speaker 1>more dense, and that actually raises the speed of sound.

0:30:40.080 --> 0:30:43.080
<v Speaker 1>So then the local flow becomes subsonic. So you get

0:30:43.200 --> 0:30:46.960
<v Speaker 1>supersonic shockwaves, which then actually becomes subsonic, and so it

0:30:47.000 --> 0:30:51.200
<v Speaker 1>creates this really complex structure and these really interesting patterns

0:30:51.200 --> 0:30:54.480
<v Speaker 1>of density. It's really hard to model because it's so chaotic.

0:30:54.960 --> 0:30:58.800
<v Speaker 2>So in order to hear sound, you need like molecules

0:30:58.840 --> 0:31:00.800
<v Speaker 2>to transmit it. So like if you were out there,

0:31:00.840 --> 0:31:05.120
<v Speaker 2>would you be hearing these particles or or not?

0:31:05.160 --> 0:31:09.479
<v Speaker 1>Really you can technically scream and be heard in the

0:31:09.480 --> 0:31:13.720
<v Speaker 1>interstellar medium, it would be very faint and very very slow. Right, Okay,

0:31:13.840 --> 0:31:15.600
<v Speaker 1>you could hear these things, I can tell you what

0:31:15.640 --> 0:31:20.080
<v Speaker 1>they would sound like. You know, probably like shh cool.

0:31:20.160 --> 0:31:23.000
<v Speaker 2>Okay, interesting, I don't know why, But in my mind,

0:31:23.000 --> 0:31:26.040
<v Speaker 2>I'd imagine the interstellar space is being like a quiet, calm,

0:31:26.120 --> 0:31:28.800
<v Speaker 2>still place, which is probably silly because you know, like

0:31:28.840 --> 0:31:31.080
<v Speaker 2>solar winds keep things moving. There's probably nowhere that in

0:31:31.080 --> 0:31:34.080
<v Speaker 2>space that's actually super still, But I hadn't imagined it

0:31:34.120 --> 0:31:36.000
<v Speaker 2>being super turbulent like this.

0:31:36.120 --> 0:31:39.400
<v Speaker 1>So yeah, it's really turbulent. And you know, on time

0:31:39.440 --> 0:31:41.320
<v Speaker 1>scales that we don't usually think about, but if you

0:31:41.640 --> 0:31:44.320
<v Speaker 1>played a movie, you know, where a million years passes

0:31:44.360 --> 0:31:47.720
<v Speaker 1>in a second, it would look like bubbling, frothing tea

0:31:47.880 --> 0:31:50.440
<v Speaker 1>or something. You know, it's a lot of stuff going on.

0:31:51.200 --> 0:31:53.200
<v Speaker 1>And the most interesting stuff that goes on is that

0:31:53.240 --> 0:31:56.320
<v Speaker 1>when you get dense regions, you get star formation. Right,

0:31:56.840 --> 0:31:59.400
<v Speaker 1>if you have a clump of gas and it cools

0:31:59.480 --> 0:32:02.440
<v Speaker 1>down and then one of those grains of dust can

0:32:02.480 --> 0:32:06.040
<v Speaker 1>start to gather other stuff near it. It's important that's cool, remember,

0:32:06.320 --> 0:32:08.560
<v Speaker 1>because if things are really really hot, and that means

0:32:08.600 --> 0:32:11.520
<v Speaker 1>they're moving fast and then gravity has no chance to

0:32:11.520 --> 0:32:13.800
<v Speaker 1>pull them together. But if things are cool, that means

0:32:13.840 --> 0:32:17.080
<v Speaker 1>they're slow moving and gravity can gather dust grains together

0:32:17.200 --> 0:32:20.080
<v Speaker 1>little bits at a time. They stick together, they start

0:32:20.120 --> 0:32:22.600
<v Speaker 1>forming bigger and bigger stuff and that's when you get

0:32:22.600 --> 0:32:25.840
<v Speaker 1>gravitational collapse leads to a runaway effect. You get more gravity,

0:32:26.200 --> 0:32:28.400
<v Speaker 1>and then you get a star forming and there stuff

0:32:28.440 --> 0:32:31.800
<v Speaker 1>around it starts to swirl around it to a protoplanetary disc.

0:32:32.160 --> 0:32:34.600
<v Speaker 1>And that's how a star is born. It's born from

0:32:34.800 --> 0:32:38.200
<v Speaker 1>denser regions in the interstellar medium, and those regions come

0:32:38.240 --> 0:32:41.520
<v Speaker 1>from the turbulence. So the structure in the interstellar medium

0:32:41.680 --> 0:32:43.200
<v Speaker 1>is the reason we have stars.

0:32:43.840 --> 0:32:46.880
<v Speaker 2>The structure in the interstellar medium. But don't you only

0:32:46.920 --> 0:32:51.480
<v Speaker 2>have interstellar medium because it's the region between pre existing stars.

0:32:52.000 --> 0:32:56.040
<v Speaker 1>Yeah, there's sort of a circular definition there, but yeah,

0:32:56.080 --> 0:32:59.040
<v Speaker 1>the interstellar medium can make new stars and then it's

0:32:59.040 --> 0:33:00.480
<v Speaker 1>no longer the interstellar medium.

0:33:00.600 --> 0:33:04.560
<v Speaker 2>Okay, So you can imagine this process going on infinitely

0:33:04.560 --> 0:33:06.640
<v Speaker 2>many times, and then you just have an infinite number

0:33:06.640 --> 0:33:09.120
<v Speaker 2>of suns. So how often does this process happen?

0:33:09.320 --> 0:33:12.120
<v Speaker 1>So it depends a lot on the details of the

0:33:12.160 --> 0:33:15.600
<v Speaker 1>temperature of the cloud and the composition. But when it happens,

0:33:15.600 --> 0:33:17.479
<v Speaker 1>it happens a lot. Like you get a lot of

0:33:17.520 --> 0:33:20.520
<v Speaker 1>stars all born in one of the neighborhood together. And

0:33:20.560 --> 0:33:23.680
<v Speaker 1>this is why, for example, stars are very often found

0:33:23.680 --> 0:33:27.240
<v Speaker 1>in binary systems like pairs of stars gravitationally bound to

0:33:27.280 --> 0:33:31.040
<v Speaker 1>each other, or even briefly trinary systems or more long

0:33:31.080 --> 0:33:33.240
<v Speaker 1>lived systems where you have like a binary star and

0:33:33.320 --> 0:33:36.360
<v Speaker 1>another one that's more distant, so that it's like effectively

0:33:36.360 --> 0:33:39.120
<v Speaker 1>a binary system. So you have these regions of star

0:33:39.160 --> 0:33:42.480
<v Speaker 1>formation where a huge cloud meets these requirements where you

0:33:42.480 --> 0:33:45.000
<v Speaker 1>have like little dense grains and the whole thing is

0:33:45.040 --> 0:33:48.400
<v Speaker 1>cold enough, and how often it happens depends a lot

0:33:48.480 --> 0:33:51.720
<v Speaker 1>on the history of your galaxy. There's actually an interplay

0:33:51.760 --> 0:33:54.160
<v Speaker 1>between the stars and the interstelling medium, which we're going

0:33:54.240 --> 0:33:56.840
<v Speaker 1>to talk about, because the stars push back and form

0:33:56.920 --> 0:34:00.480
<v Speaker 1>these bubbles, and so it's a whole complex of all thing.

0:34:00.560 --> 0:34:03.520
<v Speaker 1>And the rate at which stars form changes a lot

0:34:03.640 --> 0:34:06.120
<v Speaker 1>where you are in the galaxy and over time, and

0:34:06.160 --> 0:34:09.719
<v Speaker 1>it's not something we fully understand. Like some galaxies out

0:34:09.760 --> 0:34:12.719
<v Speaker 1>there have stopped forming stars at all, and some of

0:34:12.760 --> 0:34:15.480
<v Speaker 1>them are still making stars and this is called quenching,

0:34:15.960 --> 0:34:17.840
<v Speaker 1>and it's not something that's fully understood.

0:34:18.160 --> 0:34:20.080
<v Speaker 2>All right, well, we still haven't gotten to the bubbles.

0:34:20.120 --> 0:34:21.440
<v Speaker 2>How do we get closer to bubbles?

0:34:21.760 --> 0:34:24.120
<v Speaker 1>Yeah, so you have the interstellar medium. You got these

0:34:24.160 --> 0:34:26.560
<v Speaker 1>clouds of gas. Sometimes they collapse and form a star.

0:34:27.000 --> 0:34:29.080
<v Speaker 1>What happens when you make a star is that it

0:34:29.120 --> 0:34:33.000
<v Speaker 1>pushes back against the interstellar medium, right, Like our Sun

0:34:33.080 --> 0:34:35.800
<v Speaker 1>has a solar wind, and that's pushing back. The reason

0:34:35.840 --> 0:34:38.000
<v Speaker 1>we call it a solar system is it's the region

0:34:38.040 --> 0:34:40.920
<v Speaker 1>where our solar wind dominates. So now you have this

0:34:41.040 --> 0:34:44.799
<v Speaker 1>cavity inside the interstellar medium, right, And so the Sun

0:34:44.880 --> 0:34:47.239
<v Speaker 1>basically makes like a little bubble, which we call the

0:34:47.239 --> 0:34:51.279
<v Speaker 1>heliosphere by pushing back against the interstellar medium. So now

0:34:51.360 --> 0:34:53.520
<v Speaker 1>imagine you have a bunch of stars, each with their

0:34:53.560 --> 0:34:56.640
<v Speaker 1>little bubbles, and one of them goes supernova, right, So

0:34:56.719 --> 0:34:59.800
<v Speaker 1>this blows out a huge region inside the ism, and

0:34:59.840 --> 0:35:03.279
<v Speaker 1>this can create a superbubble that's like hundreds of light

0:35:03.360 --> 0:35:07.320
<v Speaker 1>years across. Because remember a supernova is the collapse of

0:35:07.320 --> 0:35:10.319
<v Speaker 1>a star of gravitationally, which then bounces back out and

0:35:10.400 --> 0:35:13.440
<v Speaker 1>dumps an enormous amount of energy. A single supernova can

0:35:13.480 --> 0:35:16.440
<v Speaker 1>be brighter than the entire galaxy and it doesn't just

0:35:16.440 --> 0:35:18.800
<v Speaker 1>put out photons. That also shoots out a huge number

0:35:18.840 --> 0:35:19.520
<v Speaker 1>of particles.

0:35:19.760 --> 0:35:24.040
<v Speaker 2>How many light years across is our solar system?

0:35:24.239 --> 0:35:26.919
<v Speaker 1>So our solar system is like one or two light

0:35:27.000 --> 0:35:30.440
<v Speaker 1>years in radius, okay, right, So it's pretty small. But

0:35:30.480 --> 0:35:33.120
<v Speaker 1>then a supernova can make a bubble that's like hundreds

0:35:33.120 --> 0:35:36.439
<v Speaker 1>of light years across. And if there's multiple supernova, because

0:35:36.440 --> 0:35:39.040
<v Speaker 1>remember stars are formed in bunches, and that means they

0:35:39.040 --> 0:35:41.600
<v Speaker 1>can also go supernova in bunches they have like their

0:35:41.600 --> 0:35:44.239
<v Speaker 1>cycles all synchronized. Oh boy, then you can get a

0:35:44.360 --> 0:35:47.480
<v Speaker 1>really big bubble that lasts for like tens of millions

0:35:47.480 --> 0:35:48.000
<v Speaker 1>of years.

0:35:48.600 --> 0:35:51.399
<v Speaker 2>Okay, so the bubbles that we're talking about then are

0:35:52.360 --> 0:35:56.799
<v Speaker 2>solar winds of some sort blowing interstellar medium out, and

0:35:56.840 --> 0:35:58.960
<v Speaker 2>that is the bubble. These are not the fun bubbles

0:35:58.960 --> 0:36:00.800
<v Speaker 2>that I was imagining, Daniel.

0:36:02.120 --> 0:36:04.160
<v Speaker 1>So you get little bubbles from solar winds, but you

0:36:04.200 --> 0:36:07.080
<v Speaker 1>really get the super bubbles from a bunch of supernova's

0:36:07.120 --> 0:36:10.880
<v Speaker 1>all going off at once and making these really vast bubbles.

0:36:11.200 --> 0:36:14.160
<v Speaker 1>It's super cool. Also, if one happens near the edge

0:36:14.200 --> 0:36:17.840
<v Speaker 1>of the galaxy, Like the galaxy is a big disc, right,

0:36:18.080 --> 0:36:21.239
<v Speaker 1>it's like much broader than it is thick. So if

0:36:21.280 --> 0:36:23.680
<v Speaker 1>it occurs like near the top of the disk, then

0:36:23.760 --> 0:36:27.040
<v Speaker 1>essentially it creates like a hole in the galaxy. And

0:36:27.120 --> 0:36:29.960
<v Speaker 1>they call it a galactic chimney because in hot gas

0:36:30.000 --> 0:36:33.520
<v Speaker 1>from inside the galaxy basically vents out from the galaxy,

0:36:34.040 --> 0:36:35.520
<v Speaker 1>so you have like a little spurt.

0:36:35.800 --> 0:36:38.440
<v Speaker 2>So the question that we're answering today is do we

0:36:38.480 --> 0:36:41.000
<v Speaker 2>live in a super bubble? But timing's got to matter too,

0:36:41.080 --> 0:36:43.000
<v Speaker 2>right now, if you get a bunch of stars going

0:36:43.040 --> 0:36:46.680
<v Speaker 2>supernova all at once to make your super bubble, you

0:36:46.719 --> 0:36:48.480
<v Speaker 2>would be dead if you were inside of the super

0:36:48.480 --> 0:36:51.200
<v Speaker 2>bubble region, right, So it's got to go super bubble,

0:36:51.360 --> 0:36:53.759
<v Speaker 2>make a bubble exact, and then a planet needs to

0:36:53.840 --> 0:36:57.120
<v Speaker 2>like wander in or get captured and then become habitable,

0:36:57.800 --> 0:37:00.360
<v Speaker 2>and then you find yourself inside the super bubble. That

0:37:00.360 --> 0:37:01.759
<v Speaker 2>would have to work, right, okay.

0:37:01.520 --> 0:37:03.719
<v Speaker 1>Right, And remember, our Solar system has existed for like

0:37:03.880 --> 0:37:06.640
<v Speaker 1>almost five billion years, but these super bubbles last for

0:37:06.760 --> 0:37:10.200
<v Speaker 1>tens of millions of years. They're very transient, and our

0:37:10.280 --> 0:37:13.719
<v Speaker 1>star is moving through the galaxy, right, and its orbit

0:37:13.760 --> 0:37:17.640
<v Speaker 1>takes hundreds of millions of years, and so they're created

0:37:17.640 --> 0:37:19.480
<v Speaker 1>by supernova. But you don't want to be there when

0:37:19.480 --> 0:37:24.000
<v Speaker 1>they're made, you're right, And so coincidentally, there is a bubble.

0:37:24.000 --> 0:37:26.799
<v Speaker 1>It's called the local bubble. It's three hundred to one

0:37:26.920 --> 0:37:30.280
<v Speaker 1>thousand light year wide. It has a much lower gas

0:37:30.320 --> 0:37:33.120
<v Speaker 1>density than the rest of the interstellar medium by like

0:37:33.280 --> 0:37:36.840
<v Speaker 1>down by ten, and it's surrounded by denser walls of

0:37:36.880 --> 0:37:40.080
<v Speaker 1>neutral gas and dust. Probably it was formed by like

0:37:40.120 --> 0:37:42.680
<v Speaker 1>maybe ten to twenty supernovas that happened over the last

0:37:42.680 --> 0:37:46.160
<v Speaker 1>ten to fifteen million years, so sort of recently on

0:37:46.239 --> 0:37:50.920
<v Speaker 1>cosmic history scales. We can't pinpoint exactly which stars they are.

0:37:50.960 --> 0:37:55.960
<v Speaker 1>Probably their stars related to the Scorpius Centaurus association of stars.

0:37:56.440 --> 0:37:58.440
<v Speaker 1>And the shape of it is kind of weird. It's

0:37:58.520 --> 0:38:01.880
<v Speaker 1>not spherical, and there's other like nearby bubbles that it

0:38:01.920 --> 0:38:06.240
<v Speaker 1>connects to called loop one, and so fortunately it formed

0:38:06.320 --> 0:38:09.439
<v Speaker 1>before we got here. Right, the Sun orbits the center

0:38:09.440 --> 0:38:12.439
<v Speaker 1>of the galaxy at like two hundred and twenty kilometers

0:38:12.440 --> 0:38:15.640
<v Speaker 1>per second and moves it like twenty five kilometers per

0:38:15.680 --> 0:38:19.720
<v Speaker 1>second relative to the interstellar medium, and so that means

0:38:19.719 --> 0:38:23.560
<v Speaker 1>that we go like twenty to thirty parsecs every million

0:38:23.640 --> 0:38:28.120
<v Speaker 1>years or so. This bubble is a few hundred parsecs across,

0:38:28.680 --> 0:38:32.520
<v Speaker 1>so seems like about fifteen million years ago the first

0:38:32.560 --> 0:38:37.000
<v Speaker 1>supernova started inflating this bubble. Five or ten million years

0:38:37.040 --> 0:38:40.440
<v Speaker 1>ago we entered the cavity, and now we're in this superbubble.

0:38:40.680 --> 0:38:44.120
<v Speaker 1>We're drifting through a little warm cloud of gas inside

0:38:44.160 --> 0:38:47.240
<v Speaker 1>this bubble, and in a couple million years we're probably

0:38:47.239 --> 0:38:50.440
<v Speaker 1>going to exit it back into the interstellar medium, which

0:38:50.480 --> 0:38:51.360
<v Speaker 1>is a little bit denser.

0:38:52.080 --> 0:38:55.440
<v Speaker 2>So when we enter the interstellar medium where there's all

0:38:55.440 --> 0:38:58.480
<v Speaker 2>of that turbulence and it's crazy, is that going to

0:38:58.520 --> 0:38:59.560
<v Speaker 2>be a bad time for us?

0:39:00.320 --> 0:39:03.399
<v Speaker 1>No, probably not, because we have the solar wind which

0:39:03.400 --> 0:39:06.960
<v Speaker 1>protects us. Were moving within our own little bubble anyway,

0:39:07.480 --> 0:39:09.840
<v Speaker 1>So it doesn't really matter that much. It's just a

0:39:09.840 --> 0:39:12.120
<v Speaker 1>way to highlight that there's a lot of stuff happening

0:39:12.160 --> 0:39:16.160
<v Speaker 1>out there, right there's turbulence and chaos and all that stuff,

0:39:16.160 --> 0:39:18.800
<v Speaker 1>and star formation and start dying and all that happens

0:39:18.920 --> 0:39:22.560
<v Speaker 1>because of this structure. Like you get stars because you

0:39:22.640 --> 0:39:26.120
<v Speaker 1>have denser regions, and then those stars blow out make

0:39:26.200 --> 0:39:29.120
<v Speaker 1>superbubbles when they die to make less dense regions. But

0:39:29.160 --> 0:39:32.720
<v Speaker 1>then those superbubbles collapse because the interior is lower density

0:39:32.719 --> 0:39:36.080
<v Speaker 1>but higher temperature, and that hot gas leaks out and

0:39:36.160 --> 0:39:39.480
<v Speaker 1>ruptures the shell, and so you get this cycle of stuff.

0:39:39.840 --> 0:39:42.120
<v Speaker 1>And so you know, you shouldn't think of the galaxy

0:39:42.160 --> 0:39:44.719
<v Speaker 1>out there between the stars is empty. In fact, it's

0:39:44.719 --> 0:39:48.880
<v Speaker 1>filled with stuff, and it's really dynamic, and the structure

0:39:49.000 --> 0:39:52.160
<v Speaker 1>out there is what determines like where stars are made

0:39:52.560 --> 0:39:56.400
<v Speaker 1>and then stars explode and replenish the interstellar medium, and

0:39:56.440 --> 0:39:59.320
<v Speaker 1>so the interplay between the stars and the interstellar medium

0:39:59.400 --> 0:40:03.279
<v Speaker 1>really determined, like, hey, is your galaxy making stars or not?

0:40:03.440 --> 0:40:05.920
<v Speaker 1>Is it to pleasing all of its gas? All this

0:40:06.000 --> 0:40:09.040
<v Speaker 1>kind of stuff is determined by this interaction between the

0:40:09.080 --> 0:40:10.760
<v Speaker 1>stars and the interstellar medium.

0:40:10.920 --> 0:40:14.239
<v Speaker 2>Huh. So we live inside of a bubble made by

0:40:14.280 --> 0:40:18.160
<v Speaker 2>our son, which is currently inside of the local super bubble.

0:40:18.239 --> 0:40:21.560
<v Speaker 1>That's right, that was made by supernovas of other stars,

0:40:21.719 --> 0:40:23.720
<v Speaker 1>fortunately before we entered this region.

0:40:24.600 --> 0:40:27.719
<v Speaker 2>Amazing exactly, And.

0:40:27.719 --> 0:40:30.560
<v Speaker 1>So that's the broader context of your life. We happen

0:40:30.600 --> 0:40:32.920
<v Speaker 1>to be living inside this bubble, and now you.

0:40:32.960 --> 0:40:35.400
<v Speaker 2>Know all about it, that's right. And we hope that

0:40:35.440 --> 0:40:38.360
<v Speaker 2>you don't stub your toes on any galactic dust or

0:40:38.440 --> 0:40:41.200
<v Speaker 2>happen to get dust of any sort inside of your

0:40:41.239 --> 0:40:44.360
<v Speaker 2>gallbladder or kidneys or anything else. We wish you health.

0:40:44.360 --> 0:40:47.520
<v Speaker 2>And this is not a great transition. But man, it

0:40:47.640 --> 0:40:49.400
<v Speaker 2>hurt to laugh at Daniel's jokes today.

0:40:50.160 --> 0:40:51.879
<v Speaker 1>I try to hold back. I really really did.

0:40:52.280 --> 0:40:54.600
<v Speaker 2>I appreciate it. Daniel. You can't help yourself. You're just

0:40:54.640 --> 0:40:55.200
<v Speaker 2>a funny guy.

0:40:57.160 --> 0:41:00.920
<v Speaker 1>Looks, Aren't everything right ready?

0:41:09.040 --> 0:41:12.880
<v Speaker 2>Daniel and Kelly's Extraordinary Universe is produced by iHeartRadio. We

0:41:12.920 --> 0:41:14.319
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0:41:14.440 --> 0:41:17.360
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0:41:30.560 --> 0:41:33.759
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0:41:32.800 --> 0:41:34.880
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