WEBVTT - What's hidden inside planets?

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<v Speaker 1>When we set out to understand the universe, we usually

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<v Speaker 1>start by looking up. After all, that's where the best

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<v Speaker 1>views are of the glittery cosmos stretched across billions of miles.

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<v Speaker 1>We wonder, are we alone? Is there anyone up there

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<v Speaker 1>looking back at us? But what if the best way

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<v Speaker 1>to find answers to questions about what's up there is

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<v Speaker 1>actually to look down under our feet. Hi, I'm Daniel.

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<v Speaker 1>I'm a particle physicist and a professor at UC Irvine,

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<v Speaker 1>and I desperately want to know who's out there in

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<v Speaker 1>the universe and if they are wondering the same things

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<v Speaker 1>we are. And Welcome to the podcast Daniel and Horace

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<v Speaker 1>Explain the Universe in which we do just that, wonder

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<v Speaker 1>about the nature of the universe and try to explain

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<v Speaker 1>all of it to you. Regular listeners the podcast, know

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<v Speaker 1>that I am desperate to understand the nature of the universe,

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<v Speaker 1>how it all works, and to explain all of that

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<v Speaker 1>knowledge and all of that confusion to you. One of

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<v Speaker 1>the deepest questions we wrestle with on the pod is

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<v Speaker 1>not just about the universe, but kind of about ourselves.

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<v Speaker 1>How weird? Are we are? There more like us out

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<v Speaker 1>there in the universe, or are we alone? How rare

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<v Speaker 1>and special is the Earth anyway? Are we one of

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<v Speaker 1>a kind out of a trillion planets, or are we

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<v Speaker 1>one of many rocky balls covered in Curious Life. We're

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<v Speaker 1>frustratingly limited by what we can learn about distant planets,

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<v Speaker 1>though we're doing our best. But something we can do

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<v Speaker 1>right now is drill deeper into our own planet, understand

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<v Speaker 1>the forces that shaped it and whether those are finely

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<v Speaker 1>balanced in a rare way or naturally in harmony, in

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<v Speaker 1>a way we'll find everywhere in the universe. So today

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<v Speaker 1>on the podcast, we'll be answering the question what's hidden

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<v Speaker 1>inside planets? And to help me explore this fascinating topic,

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<v Speaker 1>I'm pleasing to be speaking to Professor Sabina Stanley, author

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<v Speaker 1>of a very recent book of that same title. All right, well,

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<v Speaker 1>then it's my great pleasure to introduce the podcast Professor

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<v Speaker 1>Sabina Stanley. She's the Bloomberg Distinguished Professor of Planetary Physics

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<v Speaker 1>at Johns Hopkins University, where she focuses on magnetic fields

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<v Speaker 1>and other geophysical elements as a means of studying the

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<v Speaker 1>interiors of planets, moons, and asteroids. She's an Alfred Peasloan

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<v Speaker 1>Research Fellow, and has also received the William Gilbert Award

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<v Speaker 1>of the American Geophysical Union. Sabina, Welcome to the podcast,

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<v Speaker 1>and thank you for coming to talk to us.

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<v Speaker 2>Thanks so much for having me.

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<v Speaker 1>So one thing we always wonder about as we look

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<v Speaker 1>out into the night sky is all the other planets

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<v Speaker 1>that are out there. Of course we can't study mnie

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<v Speaker 1>them up close, and so often on this podcast we've

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<v Speaker 1>tried to dig into what's under our feet, the mysteries

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<v Speaker 1>that are right here in our Earth. And so I

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<v Speaker 1>really enjoyed your recent book, What's Hidden Inside Planets, and

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<v Speaker 1>I'd love to talk to you about what's in our planet.

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<v Speaker 1>Could you start us off by taking us sort of

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<v Speaker 1>on a brief tour of like what is under our feet,

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<v Speaker 1>layer by layer, all the way down to the core.

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<v Speaker 2>Yeah, absolutely, great question.

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<v Speaker 3>So I think it's interesting to note that when you

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<v Speaker 3>start on the surface, as you go deeper and deeper,

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<v Speaker 3>stuff gets kind of weirder and weirder and much more

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<v Speaker 3>different than what we're used to on the surface.

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<v Speaker 2>So we start on the crust.

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<v Speaker 3>This is where we live, This is where all the

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<v Speaker 3>stuff happens that we're used to crust can vary in

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<v Speaker 3>thickness five about you know, five kilometers depth to almost

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<v Speaker 3>one hundred kilometers depth. But under that you get to

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<v Speaker 3>the mantle that's also still mostly rocky, the type of

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<v Speaker 3>rocks that are rich in magnesium and silicates, but still

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<v Speaker 3>what we would recognize as rocks. So about half the

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<v Speaker 3>radius of the Earth are those rocks. It goes down

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<v Speaker 3>about two thousand miles deep.

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<v Speaker 1>So what distinguishes then between the crust and the mantle.

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<v Speaker 1>Is it like how squeezed they are and how much

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<v Speaker 1>they flow, or is it a different kind of rock?

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<v Speaker 2>Great question.

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<v Speaker 3>Yeah, it's a little bit different kind of rock. So

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<v Speaker 3>essentially the crust layer of the earth. I sometimes refer

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<v Speaker 3>to it as like the scum of the earth. So

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<v Speaker 3>it's kind of like, you know, like when you're making

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<v Speaker 3>a soup and you're boiling your broth and you've got

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<v Speaker 3>all that light, floaty stuff that comes to the top.

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<v Speaker 3>So the stuff that's the most buoyant when you have

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<v Speaker 3>certain heat, thermal reactions and chemical reactions happening with rocks

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<v Speaker 3>near the surface, all of that percolates up to the

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<v Speaker 3>top and that ends up becoming the crust, and then

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<v Speaker 3>sort of the stuff underneath might be less scummy, less

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<v Speaker 3>you know, it's been less reworked, and it's sort of

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<v Speaker 3>more kind of pristine rock.

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<v Speaker 1>I see, we're going to get started very quickly with

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<v Speaker 1>the food analogies.

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<v Speaker 2>Yeah, I'm sorry, it's just going to be how it goes.

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<v Speaker 3>It's going to be food involved in almost every analogy

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<v Speaker 3>I make.

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<v Speaker 2>Here.

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<v Speaker 1>Are you a big fan of soup or you a

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<v Speaker 1>cook at home?

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<v Speaker 3>So I'm a terrible cook, but I grew up in

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<v Speaker 3>a restaurant family, so I've been around sort of good

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<v Speaker 3>food my whole life.

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<v Speaker 1>All right, Well, then let's do our best to at

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<v Speaker 1>least use tasty food analogies. I don't want any want

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<v Speaker 1>to think that the earth is like a disgusting bowl

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<v Speaker 1>of soup. Maybe it's like, you know, bubbling hot cocoa,

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<v Speaker 1>and this is that delicious film that forms on top.

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<v Speaker 2>I love that so much. You don't even know. So

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<v Speaker 2>that's amazing, all right.

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<v Speaker 1>So the crust is the sort of coolest part that

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<v Speaker 1>floats to the top, and underneath that it's still rock,

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<v Speaker 1>but it's able to flow. How do we visualize that?

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<v Speaker 1>I mean, it's not like liquid lava that's flowing on

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<v Speaker 1>the surface. This is still like solid rock, but it's flowing.

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<v Speaker 1>How does solid rock flow is something I've always tried

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<v Speaker 1>to visualize and failed.

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<v Speaker 2>Yeah, So the answer to that question is very slowly.

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<v Speaker 1>Right.

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<v Speaker 3>So, yes, it's solid, but it's still deformable, right, And

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<v Speaker 3>I think we have experience with different types of solids

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<v Speaker 3>in our everyday life, and that some are more deformable

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<v Speaker 3>than other.

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<v Speaker 2>Right, Like you might have clay.

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<v Speaker 3>Clay is solid, but you can still deform it, whereas

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<v Speaker 3>a metal also is kind of deformable. But then you

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<v Speaker 3>have some rocks that are really like a diamond, really

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<v Speaker 3>hard to deform. But the rocks in the mantle, they

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<v Speaker 3>are solid, but they can be deformed, and if they

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<v Speaker 3>can be deformed, then they start being influenced by the

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<v Speaker 3>forces like gravity such that you can get them to flow.

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<v Speaker 1>I see, all right, So we have the crust and

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<v Speaker 1>we have the mantle. Both the wiz are still really rock.

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<v Speaker 1>Take us down below that, right.

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<v Speaker 3>So then you get down about halfway through the Earth

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<v Speaker 3>and you suddenly hit a very big boundary, complete change

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<v Speaker 3>of environment. Now you're at the iron core. So the

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<v Speaker 3>inner half of the planet about it's mostly made of iron.

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<v Speaker 3>There's a little bit of nickel mixed in there, and

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<v Speaker 3>about ten percent of some sort of lighter elements that

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<v Speaker 3>we have a whole sort of platter of possibilities for,

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<v Speaker 3>but we don't actually know what they are. And that

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<v Speaker 3>makes up the core. The core has two parts to it.

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<v Speaker 3>The outer port is liquid. It can flow very easily,

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<v Speaker 3>much faster timescales than the mantle, and it's really important

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<v Speaker 3>for us because that's where our magnetic field is generated

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<v Speaker 3>in that liquid iron core. Then below that, the innermost

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<v Speaker 3>thirteen hundred kilometers of our planet, is a solid iron core.

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<v Speaker 1>And so what distinguishes then the mantle, which can flow

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<v Speaker 1>but is a solid not a liquid, from the outer core,

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<v Speaker 1>which can flow but is a liquid and not a solid, Like,

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<v Speaker 1>is there really a distinction here? Are we just putting

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<v Speaker 1>labels on things?

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<v Speaker 3>When we study fluid dynamics, we talk a lot about

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<v Speaker 3>there being a spectrum of fluids. Right, nothing's ever purely

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<v Speaker 3>a solid or purely a fluid. It's all about the

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<v Speaker 3>time scales. So the mantle, for example, if you want

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<v Speaker 3>to talk about how materials flow in the mantle, a

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<v Speaker 3>parcel at the bottom of the mantle could take hundreds

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<v Speaker 3>of millions of years to make it to the top

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<v Speaker 3>of the mantle, whereas a parcel at the bottom of

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<v Speaker 3>the core could take a couple of years to get

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<v Speaker 3>the top of the core. So it's a very different

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<v Speaker 3>timescale of the flow. You could actually see changes in

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<v Speaker 3>material in the core flowing.

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<v Speaker 1>But this is also like a boundary. It's not like

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<v Speaker 1>there's a smooth, very gradual transition. There's like a line.

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<v Speaker 1>You can say, this is the core and this is

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<v Speaker 1>the mantle.

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<v Speaker 3>Yeah, And that happens because mantle, rocks, and iron in

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<v Speaker 3>the core have very different densities, and at one time

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<v Speaker 3>in the past in our planet, it was mostly molten

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<v Speaker 3>and so the heaviest stuff, when you have a bunch

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<v Speaker 3>of stuff mixed together, the heaviest stuff's going to sync

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<v Speaker 3>to the bottom. And so that's what happened in Earth.

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<v Speaker 3>All the iron, most of the irons, sunk to the

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<v Speaker 3>center of the Earth and made.

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<v Speaker 1>Up the core like the big chunks in a stew

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<v Speaker 1>or something exactly.

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<v Speaker 2>Yes, I like it.

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<v Speaker 1>So the reason that there's a boundary there and like

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<v Speaker 1>a transition or rather than just like a smooth gradation

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<v Speaker 1>from more liquid to less liquid, that reflects like the

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<v Speaker 1>phase transitions and materials. Is that right, the way that

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<v Speaker 1>like ice turns solid at some moment and doesn't just

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<v Speaker 1>like gradually become more and more solid.

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<v Speaker 3>I would say that's more representative of what kind of

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<v Speaker 3>happens at the inner core outer core boundary, so where

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<v Speaker 3>the iron becomes solid. But above that it's more kind

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<v Speaker 3>of like a maybe you go with an oil and

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<v Speaker 3>water type thing. You've got two materials with very different

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<v Speaker 3>density and very different properties, so it's really hard to

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<v Speaker 3>mix them.

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<v Speaker 1>Wonderful and tell us about how we know about this.

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<v Speaker 1>I was reading in your book this really exciting description

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<v Speaker 1>of the mantle race, basically like a parallel to the

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<v Speaker 1>space race, but into the Earth. Tell us about our

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<v Speaker 1>humanity's efforts to like literally tunnel to the center of

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<v Speaker 1>the Earth.

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<v Speaker 3>Yeah, So if you imagine you want to figure what's

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<v Speaker 3>inside the Earth, right, your first instinct might be, hey,

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<v Speaker 3>why don't we dig down as far as we can

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<v Speaker 3>and actually sample it?

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<v Speaker 2>Right?

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<v Speaker 3>And it's a great instinct. Unfortunately, it's incredibly challenging to do.

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<v Speaker 3>And that's because pressure increases so fast as you go

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<v Speaker 3>deeper inside the planet, and so do temperatures. So as

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<v Speaker 3>you can imagine, humans don't like really high pressures and temperatures.

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<v Speaker 3>Neither does equipment, and the farthest we've been able to

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<v Speaker 3>dig with sort of a really concerted effort to do so, right,

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<v Speaker 3>Like this was something on the scale of moonshot to

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<v Speaker 3>the Moon in the late sixties. This is something very

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<v Speaker 3>similar to that, And you could get only down to

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<v Speaker 3>about eight miles in depth, and the radius of the

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<v Speaker 3>Earth you're talking about four thousand miles, so tiny, tiny

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<v Speaker 3>scrape of the surface by going down that deep. Equipment

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<v Speaker 3>does not like high pressures and temperatures.

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<v Speaker 1>But how do you even get eight miles deep? I mean,

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<v Speaker 1>I remember digging in my backyard with a shovel, wondering

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<v Speaker 1>how far I could get, and it's not very far.

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<v Speaker 1>How do you get eight miles down?

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<v Speaker 3>This is like high tech technology kind of stuff. It's

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<v Speaker 3>at the limits of what we can do for drilling

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<v Speaker 3>that we do now to drill for resources, et cetera.

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<v Speaker 3>So it's a lot of fancy equipment and challenges that

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<v Speaker 3>are over met that way. So we can't dig and

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<v Speaker 3>we can't drill, But that's okay because there are other

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<v Speaker 3>ways we can figure out what's going on deeper inside

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<v Speaker 3>the earth.

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<v Speaker 1>Yeah, So tell us about some of those ways you

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<v Speaker 1>were talking in the book about diamonds, how we can

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<v Speaker 1>use diamonds to give us little snapshots of what's inside

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<v Speaker 1>the planet.

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<v Speaker 3>Yeah, so you know, it would be great if we

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<v Speaker 3>could dig down, but would it also be great if

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<v Speaker 3>the stuff down there came to us. And that's really

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<v Speaker 3>what happens with diamonds. Diamonds are produced deeper inside the Earth,

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<v Speaker 3>and then they come up to the surface, usually in

0:10:36.960 --> 0:10:41.120
<v Speaker 3>volcanic vent things known as kimber like pipes and those diamonds.

0:10:41.120 --> 0:10:43.960
<v Speaker 3>You know, Jewelers love diamonds when they're as pure as possible.

0:10:44.160 --> 0:10:47.520
<v Speaker 3>Geologists love diamonds when they're as impure as possible. So

0:10:48.040 --> 0:10:51.000
<v Speaker 3>sometimes diamonds, when they form, they can enclose a little

0:10:51.040 --> 0:10:54.360
<v Speaker 3>capsule of some of the material where they formed inside them, right,

0:10:54.400 --> 0:10:56.080
<v Speaker 3>So you might get a little bit of garnet in

0:10:56.120 --> 0:10:57.880
<v Speaker 3>the diamond or a little bit of something that was

0:10:57.920 --> 0:11:00.360
<v Speaker 3>created deeper in the earth. And when it it up,

0:11:00.360 --> 0:11:03.160
<v Speaker 3>because diamonds so strong, it actually keeps the material in

0:11:03.200 --> 0:11:06.040
<v Speaker 3>its like pristine form, So you really have this like

0:11:06.160 --> 0:11:08.040
<v Speaker 3>sample from the interior of the Earth come to the

0:11:08.080 --> 0:11:10.880
<v Speaker 3>surface for us to investigate. So that's a great way

0:11:10.920 --> 0:11:12.959
<v Speaker 3>and we've used that, for example, to figure out that

0:11:13.280 --> 0:11:16.880
<v Speaker 3>there is actually water deeper inside the Earth because we've

0:11:16.920 --> 0:11:20.120
<v Speaker 3>found water inside diamond inclusions.

0:11:20.360 --> 0:11:22.480
<v Speaker 1>It's fascinating to me though, that this thing that you

0:11:22.559 --> 0:11:24.600
<v Speaker 1>make in a high pressure environment, when you bring it

0:11:24.720 --> 0:11:28.120
<v Speaker 1>up to low pressure, it doesn't explode. Is that just

0:11:28.120 --> 0:11:29.840
<v Speaker 1>because of the incredible structure of diamond?

0:11:30.120 --> 0:11:30.400
<v Speaker 2>Yeah.

0:11:30.480 --> 0:11:33.000
<v Speaker 3>When they say diamonds are forever, that's technically not true, right,

0:11:33.000 --> 0:11:36.079
<v Speaker 3>They just have a really really long lifetime before they

0:11:36.200 --> 0:11:37.720
<v Speaker 3>revert back to their carbon phase.

0:11:37.800 --> 0:11:40.199
<v Speaker 2>So yeah, it's just a great property of diamond.

0:11:40.320 --> 0:11:41.640
<v Speaker 1>So is it's sort of like you know, you put

0:11:41.640 --> 0:11:44.000
<v Speaker 1>a pan of brownies in the oven and it changes

0:11:44.040 --> 0:11:45.720
<v Speaker 1>into something else, and when you take it out, cool

0:11:45.760 --> 0:11:47.520
<v Speaker 1>it down, it doesn't revert back into batter.

0:11:47.880 --> 0:11:49.480
<v Speaker 2>That's an excellent way of thinking about it.

0:11:49.559 --> 0:11:53.080
<v Speaker 1>Yeah, okay, And so then what have we learned from

0:11:53.120 --> 0:11:56.440
<v Speaker 1>these diamond samples? Like what's inside these diamonds that we

0:11:56.480 --> 0:11:57.959
<v Speaker 1>didn't realize other than water?

0:11:58.120 --> 0:11:59.960
<v Speaker 2>Yeah? I think water is the big thing.

0:12:00.120 --> 0:12:04.240
<v Speaker 3>Sometimes it's a lot about sort of the smaller amounts

0:12:04.240 --> 0:12:06.680
<v Speaker 3>of elements that we don't know about, Right, how much

0:12:07.080 --> 0:12:10.280
<v Speaker 3>of a particular kind of silicon down there is sulfur,

0:12:10.320 --> 0:12:12.400
<v Speaker 3>down there these kinds of questions, and those all just

0:12:12.440 --> 0:12:15.520
<v Speaker 3>help us understand what the building blocks of Earth were

0:12:15.679 --> 0:12:19.959
<v Speaker 3>when Earth formed, and what the geochemistry the kind of

0:12:20.040 --> 0:12:23.720
<v Speaker 3>chemical reactions that can occur as material descends into the Earth.

0:12:23.760 --> 0:12:27.240
<v Speaker 3>That's really where we get that information. But even with diamonds, right,

0:12:27.280 --> 0:12:30.840
<v Speaker 3>we're talking about the outermost layers of the mantle, right, diamonds.

0:12:31.120 --> 0:12:33.319
<v Speaker 3>We don't get diamonds safe from the core mantle boundary

0:12:33.360 --> 0:12:35.280
<v Speaker 3>or anywhere deeper than that. So we can't use the

0:12:35.280 --> 0:12:37.000
<v Speaker 3>diamonds to learn about the deeper parts.

0:12:37.120 --> 0:12:40.079
<v Speaker 1>Is that because diamonds aren't made deeper or because diamonds

0:12:40.120 --> 0:12:41.800
<v Speaker 1>from that far down just don't make it up to

0:12:41.800 --> 0:12:42.280
<v Speaker 1>the surface.

0:12:42.520 --> 0:12:46.000
<v Speaker 3>Mostly the latter, I think also, like if you get

0:12:46.040 --> 0:12:49.520
<v Speaker 3>carbon down there, yeah, it doesn't necessarily join into making

0:12:49.559 --> 0:12:50.560
<v Speaker 3>diamond at that depth.

0:12:50.640 --> 0:12:53.520
<v Speaker 1>All right, So there aren't like huge diamonds buried deep

0:12:53.559 --> 0:12:57.000
<v Speaker 1>in the earth that we are not on Earth, not

0:12:57.120 --> 0:12:59.959
<v Speaker 1>on Earth. Well, that was my whole motivation for digging

0:13:00.040 --> 0:13:02.600
<v Speaker 1>so deeply when I was a kid, fantasizing about revealing

0:13:02.640 --> 0:13:05.600
<v Speaker 1>some you know, boulder sized diamond. All right, So diamonds

0:13:05.600 --> 0:13:07.480
<v Speaker 1>give us one sample of what else can we do?

0:13:07.559 --> 0:13:10.320
<v Speaker 1>What about gravity? What about just studying like the variation

0:13:10.440 --> 0:13:13.440
<v Speaker 1>in Earth's gravity as we you know, orbit to planate

0:13:13.559 --> 0:13:15.319
<v Speaker 1>or look around it. What does that tell us about

0:13:15.320 --> 0:13:16.319
<v Speaker 1>what's inside the Earth.

0:13:16.400 --> 0:13:17.800
<v Speaker 3>The way I like to think about it is, you know,

0:13:17.840 --> 0:13:19.400
<v Speaker 3>if you want to figure out what's going on inside

0:13:19.440 --> 0:13:22.920
<v Speaker 3>the Earth, try and make an analogy to a human body.

0:13:23.000 --> 0:13:24.480
<v Speaker 3>Right if you if you have an ache and you

0:13:24.520 --> 0:13:27.160
<v Speaker 3>go to your doctor and you're like this hurts. Hopefully

0:13:27.160 --> 0:13:29.240
<v Speaker 3>they're not. Their first kind of instinct is not to

0:13:29.320 --> 0:13:30.840
<v Speaker 3>drill a hole in you to figure that out. Right,

0:13:30.880 --> 0:13:33.920
<v Speaker 3>There are ways that they can use different fields and

0:13:33.960 --> 0:13:36.480
<v Speaker 3>different scans to figure out what's wrong with your insides,

0:13:36.520 --> 0:13:38.080
<v Speaker 3>And we can do the same thing for the inside

0:13:38.080 --> 0:13:41.000
<v Speaker 3>of the Earth. So we can scan gravity as you mentioned,

0:13:41.040 --> 0:13:43.280
<v Speaker 3>that's one, Magnetic fields is another one.

0:13:43.440 --> 0:13:45.160
<v Speaker 2>And we can also determine.

0:13:44.800 --> 0:13:47.599
<v Speaker 3>Properties of waves that travel through the Earth from earthquakes

0:13:47.600 --> 0:13:50.280
<v Speaker 3>through seismology. So we can use all these scanning techniques

0:13:50.280 --> 0:13:52.160
<v Speaker 3>to figure out what's going on deeper inside the Earth.

0:13:52.200 --> 0:13:54.120
<v Speaker 1>So what do you mean by using gravity? Is it

0:13:54.200 --> 0:13:56.960
<v Speaker 1>just like measuring the variations of gravity so that we

0:13:57.080 --> 0:13:59.439
<v Speaker 1>understand how the Earth is not a perfect sphere or

0:13:59.640 --> 0:14:02.240
<v Speaker 1>how they'rear is not homogeneous in density. What is it

0:14:02.280 --> 0:14:02.880
<v Speaker 1>we're learning?

0:14:03.000 --> 0:14:03.800
<v Speaker 2>Yeah, great question.

0:14:03.960 --> 0:14:06.440
<v Speaker 3>So, yeah, it really is the fact that both isn't

0:14:06.440 --> 0:14:11.040
<v Speaker 3>a perfect sphere and has some inhomogeneous material below it. Right,

0:14:11.080 --> 0:14:13.040
<v Speaker 3>So if you were walking around with a griviminter that

0:14:13.080 --> 0:14:15.679
<v Speaker 3>could measure gravity and it was really really good and

0:14:15.720 --> 0:14:18.480
<v Speaker 3>you walked around, you would get slightly different values everywhere

0:14:18.480 --> 0:14:20.920
<v Speaker 3>you walk, and that would be determined by the mass

0:14:20.960 --> 0:14:23.960
<v Speaker 3>directly under your feet. And so we can use that information.

0:14:24.120 --> 0:14:27.400
<v Speaker 3>We have spacecraft that orbit the Earth that measure Earth's

0:14:27.400 --> 0:14:30.120
<v Speaker 3>gravity feel to really high precision, and we can use

0:14:30.160 --> 0:14:32.640
<v Speaker 3>that to figure out what is the distribution of density

0:14:32.640 --> 0:14:34.600
<v Speaker 3>inside the Earth. And that kind of allows us to

0:14:34.680 --> 0:14:37.120
<v Speaker 3>kind of image what's going on. Where's the denser stuff

0:14:37.120 --> 0:14:38.720
<v Speaker 3>in the Earth, where's the lighter stuff? And we can

0:14:38.720 --> 0:14:42.240
<v Speaker 3>actually see things like convection cells in the mantle and

0:14:42.480 --> 0:14:45.920
<v Speaker 3>plumes of magma coming up for volcanoes, things like this.

0:14:46.160 --> 0:14:48.640
<v Speaker 1>But gravity is such a weak force. How do you

0:14:49.000 --> 0:14:53.680
<v Speaker 1>identify these variations in density with such an incredibly weak force.

0:14:53.720 --> 0:14:55.360
<v Speaker 1>They must be pretty big effects.

0:14:55.640 --> 0:14:58.120
<v Speaker 3>They aren't. They are very very tiny effect. We're just

0:14:58.240 --> 0:14:59.400
<v Speaker 3>really good at measuring them.

0:15:00.120 --> 0:15:02.720
<v Speaker 1>Emitter, you mentioned this might seem like a weird object

0:15:02.840 --> 0:15:05.120
<v Speaker 1>or listeners. But I guess, like my bathroom scale is

0:15:05.120 --> 0:15:06.800
<v Speaker 1>a gravi emitter. If I walked around the Earth with

0:15:06.840 --> 0:15:10.120
<v Speaker 1>my bathroom scale, I would measure different weights before and

0:15:10.200 --> 0:15:12.920
<v Speaker 1>after lunch, of course, but also if I didn't need anything,

0:15:13.280 --> 0:15:15.880
<v Speaker 1>or I user reference mass, then I guess I would

0:15:15.880 --> 0:15:18.320
<v Speaker 1>measure different accelerations due to gravity.

0:15:18.480 --> 0:15:18.680
<v Speaker 2>Yeah.

0:15:18.680 --> 0:15:20.920
<v Speaker 3>Absolutely, And if you are someone on the surface taking

0:15:20.920 --> 0:15:24.640
<v Speaker 3>gravity measurements, that's exactly the kind of instrument you would use. Interestingly,

0:15:25.120 --> 0:15:28.360
<v Speaker 3>once we get into orbiting around a planet like Earth

0:15:28.560 --> 0:15:31.240
<v Speaker 3>to take measurements, we use a completely different technique. We

0:15:31.360 --> 0:15:34.239
<v Speaker 3>basically use the fact that if we have a spacecraft

0:15:34.240 --> 0:15:36.600
<v Speaker 3>in orbit around the Earth, we know it's in orbit

0:15:36.640 --> 0:15:40.120
<v Speaker 3>around the Earth, and its orbital speed and altitude is

0:15:40.160 --> 0:15:42.600
<v Speaker 3>completely determined by the mass of the planet.

0:15:42.680 --> 0:15:44.080
<v Speaker 2>So we can use things.

0:15:43.880 --> 0:15:47.080
<v Speaker 3>Like two spacecraft just slightly at different locations from each

0:15:47.080 --> 0:15:49.360
<v Speaker 3>other kind of moving around, and we can use the

0:15:49.440 --> 0:15:52.400
<v Speaker 3>distance between the two spacecraft as like a proxy for

0:15:52.480 --> 0:15:54.640
<v Speaker 3>how much g is right where they are, how much

0:15:54.640 --> 0:15:56.360
<v Speaker 3>the gravity is right where they are. So that's actually

0:15:56.360 --> 0:15:58.080
<v Speaker 3>how it's done in practice with spacecraft.

0:15:58.160 --> 0:16:00.640
<v Speaker 1>Wow, that's incredible, And how sensitive are they? I mean,

0:16:00.880 --> 0:16:03.280
<v Speaker 1>like one part in a thousand, one part in a million.

0:16:03.160 --> 0:16:05.200
<v Speaker 2>Yeah, one part in a million. That's where we're getting to.

0:16:05.360 --> 0:16:07.400
<v Speaker 1>Wow, So they can really tell if I've eaten lunch.

0:16:07.600 --> 0:16:09.600
<v Speaker 1>Some spacecraft up there can tell that the mass of

0:16:09.600 --> 0:16:10.640
<v Speaker 1>the Earth has changed.

0:16:11.200 --> 0:16:13.520
<v Speaker 3>One thing they're actually used for. So the Grace satellites,

0:16:13.560 --> 0:16:16.560
<v Speaker 3>which orbited Earth for about ten years, one of their

0:16:16.600 --> 0:16:19.600
<v Speaker 3>main applications was to follow water flow on the surface,

0:16:19.640 --> 0:16:21.840
<v Speaker 3>so you could see, for example, when water was filling

0:16:21.840 --> 0:16:25.560
<v Speaker 3>reservoirs underground reservoirs in certain parts of the country or

0:16:25.560 --> 0:16:27.600
<v Speaker 3>different countries if you wanted to see are we going

0:16:27.640 --> 0:16:30.200
<v Speaker 3>to have a drought, are we in a rainstorm season,

0:16:30.280 --> 0:16:31.880
<v Speaker 3>or what's the water situation going on here?

0:16:31.920 --> 0:16:34.240
<v Speaker 2>So we can even use gravity to tract climate change.

0:16:34.360 --> 0:16:37.240
<v Speaker 1>Wow, that sounds like modern day divining rods. But you're

0:16:37.280 --> 0:16:40.160
<v Speaker 1>actually using science to find the water underground. That's incredible,

0:16:40.200 --> 0:16:42.280
<v Speaker 1>all right, So gravity's one way to do it. You

0:16:42.320 --> 0:16:46.080
<v Speaker 1>also mentioned seismic probes. These are like waves inside the earth.

0:16:46.160 --> 0:16:48.120
<v Speaker 1>How do we use that to see what's going on?

0:16:48.480 --> 0:16:51.760
<v Speaker 3>So every time there's an earthquake, it's like sort of

0:16:52.160 --> 0:16:54.120
<v Speaker 3>something kind of punched the inside of the Earth at

0:16:54.160 --> 0:16:55.920
<v Speaker 3>some point and it causes the Earth to ring. It

0:16:55.960 --> 0:16:59.640
<v Speaker 3>causes waves to travel through the interior of the Earth

0:17:00.120 --> 0:17:02.360
<v Speaker 3>and on the surface of the Earth. If we put

0:17:02.400 --> 0:17:04.359
<v Speaker 3>out a bunch of instruments that can kind of measure

0:17:04.359 --> 0:17:08.119
<v Speaker 3>the shaking, so seismographs, then we can figure out a

0:17:08.119 --> 0:17:08.679
<v Speaker 3>few things.

0:17:08.560 --> 0:17:09.920
<v Speaker 2>About the earthquake waves.

0:17:09.960 --> 0:17:12.600
<v Speaker 3>We can figure out when they arrive at different locations

0:17:12.640 --> 0:17:14.919
<v Speaker 3>around the planet, and how big the waves are, the

0:17:14.920 --> 0:17:16.360
<v Speaker 3>amplitude of the waves.

0:17:16.400 --> 0:17:17.440
<v Speaker 2>And the speed.

0:17:17.480 --> 0:17:20.760
<v Speaker 3>The timing of when the waves arrive is completely directly

0:17:20.800 --> 0:17:24.160
<v Speaker 3>related to the material properties that the waves traveled through.

0:17:24.520 --> 0:17:26.560
<v Speaker 3>So for example, we can figure out the density of

0:17:26.640 --> 0:17:29.959
<v Speaker 3>material that a wave traveled safe from. Let's say an

0:17:29.960 --> 0:17:33.439
<v Speaker 3>earthquake happens in California and the wave travels up to

0:17:34.760 --> 0:17:37.919
<v Speaker 3>Seattle in Washington. You can use that to figure out

0:17:38.000 --> 0:17:40.919
<v Speaker 3>kind of what's the material just under the surface there,

0:17:40.960 --> 0:17:43.320
<v Speaker 3>Whereas if you try to go across the globe to

0:17:43.359 --> 0:17:45.600
<v Speaker 3>another part on the other side, the waves might travel

0:17:45.640 --> 0:17:48.159
<v Speaker 3>through the entire planet and we could actually sample the

0:17:48.200 --> 0:17:49.200
<v Speaker 3>material in the.

0:17:49.119 --> 0:17:50.120
<v Speaker 2>Core for example.

0:17:50.200 --> 0:17:52.320
<v Speaker 3>So you can use all those different measurements. The more

0:17:52.480 --> 0:17:54.720
<v Speaker 3>locations you have on the Earth for these seismic measurements

0:17:54.800 --> 0:17:56.800
<v Speaker 3>to be made, the more you can kind of discern

0:17:57.520 --> 0:17:59.440
<v Speaker 3>what is the lateral structure of the.

0:17:59.320 --> 0:18:00.000
<v Speaker 2>Interior of the Earth.

0:18:00.320 --> 0:18:02.359
<v Speaker 1>And we're really talking about sound waves, right, These are

0:18:02.359 --> 0:18:05.120
<v Speaker 1>pressure waves in the rock, and so we can think

0:18:05.160 --> 0:18:08.880
<v Speaker 1>about how denser materials have sound travel faster, and less

0:18:08.880 --> 0:18:11.760
<v Speaker 1>dense materials sound travels lower. So you're measuring the density

0:18:12.320 --> 0:18:14.840
<v Speaker 1>of the material by measuring the speed of sound. But again,

0:18:14.880 --> 0:18:17.920
<v Speaker 1>these are rocks that are like pushing on each other, right,

0:18:17.960 --> 0:18:20.640
<v Speaker 1>Like sound waves through rock is a very weird thing

0:18:20.680 --> 0:18:21.200
<v Speaker 1>to think about.

0:18:21.520 --> 0:18:23.639
<v Speaker 3>Yeah, absolutely, So there are the sound waves that The

0:18:23.680 --> 0:18:26.080
<v Speaker 3>other type of wave that goes through are these sheer waves.

0:18:26.080 --> 0:18:29.359
<v Speaker 3>So those are kind of more like waves you'd experience

0:18:29.400 --> 0:18:31.880
<v Speaker 3>in a fluid, let's say, or not in fluid, sorry,

0:18:31.920 --> 0:18:34.160
<v Speaker 3>waves that you would experience if you try to kind

0:18:34.200 --> 0:18:36.320
<v Speaker 3>of bend peanut butter or something like that. Right, So

0:18:36.320 --> 0:18:38.840
<v Speaker 3>there's multiple kinds of waves, and some of them are

0:18:39.920 --> 0:18:43.080
<v Speaker 3>very diagnostic of what's going on in certain types of materials.

0:18:43.240 --> 0:18:45.399
<v Speaker 1>Well, I never thought we'd be talking about peanut butter waves,

0:18:45.440 --> 0:18:48.119
<v Speaker 1>but here we are. So when did we get this picture, Like,

0:18:48.280 --> 0:18:50.440
<v Speaker 1>what is the first technique that really gave us a

0:18:50.520 --> 0:18:52.720
<v Speaker 1>view of the inside of the earth. Was it the

0:18:52.800 --> 0:18:54.640
<v Speaker 1>seismographs or is it something else.

0:18:54.880 --> 0:18:55.880
<v Speaker 2>That's a good question.

0:18:56.119 --> 0:18:58.320
<v Speaker 3>It's not like there was a sun moment where suddenly

0:18:58.320 --> 0:18:59.560
<v Speaker 3>we had this picture of the Earth. I think we

0:18:59.680 --> 0:19:03.080
<v Speaker 3>develop our understanding to higher and higher precision as time

0:19:03.119 --> 0:19:03.399
<v Speaker 3>went on.

0:19:03.920 --> 0:19:05.560
<v Speaker 2>Right, I think early studies.

0:19:05.240 --> 0:19:08.040
<v Speaker 3>Of gravity, going back to Newton, let's say, was able

0:19:08.080 --> 0:19:10.080
<v Speaker 3>to tell us this is the mass of the Earth,

0:19:10.119 --> 0:19:12.240
<v Speaker 3>and then you could take, for example, samples of crustal

0:19:12.320 --> 0:19:15.040
<v Speaker 3>rocks and figure out what their density was and infer, hey,

0:19:15.040 --> 0:19:17.159
<v Speaker 3>there must be a lot more mass deeper in the center.

0:19:17.240 --> 0:19:19.880
<v Speaker 3>So that was kind of first order information you might

0:19:19.920 --> 0:19:23.399
<v Speaker 3>get so through both seismology. So early nineteen hundreds was

0:19:23.440 --> 0:19:25.880
<v Speaker 3>when we were doing some really great seismology figuring out

0:19:26.280 --> 0:19:28.560
<v Speaker 3>things like, oh, look we have a core. Right, that

0:19:28.720 --> 0:19:30.840
<v Speaker 3>was where the core was first discovered. The inner core

0:19:30.960 --> 0:19:33.440
<v Speaker 3>was discovered in the early nineteen hundreds. The first sort

0:19:33.440 --> 0:19:37.000
<v Speaker 3>of real profile of density through the Earth happened, I

0:19:37.040 --> 0:19:38.760
<v Speaker 3>think it was in the seventies with what was called

0:19:38.760 --> 0:19:42.160
<v Speaker 3>the Preliminary Reference Earth Model, which really used a whole

0:19:42.200 --> 0:19:44.080
<v Speaker 3>bunch of seismic data to really kind of do an

0:19:44.119 --> 0:19:47.160
<v Speaker 3>inverse problem and figure out here's what the seismic wave

0:19:47.200 --> 0:19:49.159
<v Speaker 3>speed and the density has to be at every depth

0:19:49.440 --> 0:19:51.280
<v Speaker 3>the in sort of like a won d earth. So

0:19:51.320 --> 0:19:54.080
<v Speaker 3>that was a big step forward there too. But at

0:19:54.119 --> 0:19:56.479
<v Speaker 3>the same time, gravity was being used, and so we

0:19:56.480 --> 0:19:58.359
<v Speaker 3>were getting pictures from different types.

0:19:58.119 --> 0:20:01.000
<v Speaker 1>Of information, But were the only a few hundred years

0:20:01.000 --> 0:20:03.240
<v Speaker 1>that we've had any sort of reasonable idea of what's

0:20:03.320 --> 0:20:05.160
<v Speaker 1>under our feet. And it sounds like only the last

0:20:05.200 --> 0:20:08.160
<v Speaker 1>few decades, maybe fifty years, that we've had any sort

0:20:08.160 --> 0:20:11.119
<v Speaker 1>of detailed picture of what's actually inside our own planet.

0:20:11.160 --> 0:20:14.160
<v Speaker 1>It's incredible how long we can remain ignorant about really

0:20:14.200 --> 0:20:16.240
<v Speaker 1>basic science about our own lives.

0:20:16.440 --> 0:20:19.840
<v Speaker 3>Yeah, when I talk to people, I tell them geophysics

0:20:20.040 --> 0:20:22.560
<v Speaker 3>is really modern physics because all of the stuff we're

0:20:22.600 --> 0:20:24.679
<v Speaker 3>doing now is all stuff that's happened sort of in

0:20:24.680 --> 0:20:27.080
<v Speaker 3>the last sixty seventy years. So I'd like to think

0:20:27.119 --> 0:20:28.840
<v Speaker 3>of it as a modern physics.

0:20:28.520 --> 0:20:32.520
<v Speaker 1>Approach, right, And now we've extended this frontier two other planets.

0:20:32.560 --> 0:20:34.800
<v Speaker 1>We've talked in the podcast before about the Insite mission,

0:20:34.840 --> 0:20:37.440
<v Speaker 1>and I think you worked on that measuring Mars quakes

0:20:37.480 --> 0:20:41.200
<v Speaker 1>to see what's inside Mars. Did the same principles apply there?

0:20:41.320 --> 0:20:44.119
<v Speaker 3>Yes, absolutely, So the amazing thing with the Inside mission

0:20:44.359 --> 0:20:47.720
<v Speaker 3>is brought a seismometer, and that seismometer had to be

0:20:47.760 --> 0:20:50.120
<v Speaker 3>placed onto the surface of Mars so that it could

0:20:50.119 --> 0:20:53.719
<v Speaker 3>measure the ground shaking essentially, and it worked, like it

0:20:53.760 --> 0:20:55.560
<v Speaker 3>was just amazing that it worked. But it was a

0:20:55.640 --> 0:20:59.240
<v Speaker 3>very interesting experience because for most of the mission, and

0:20:59.320 --> 0:21:02.639
<v Speaker 3>especially in the big all the Mars quakes we were

0:21:02.640 --> 0:21:03.879
<v Speaker 3>seeing were quite weak.

0:21:04.280 --> 0:21:05.000
<v Speaker 2>We were looking for.

0:21:04.920 --> 0:21:07.160
<v Speaker 3>The big one, right, We're looking for the big Mars quake,

0:21:07.359 --> 0:21:09.840
<v Speaker 3>because the bigger the quake, the more ways we'll travel

0:21:09.880 --> 0:21:11.960
<v Speaker 3>through the deeper parts of Mars. And so we really

0:21:11.960 --> 0:21:14.359
<v Speaker 3>wanted to study or I really wanted to study the core,

0:21:14.720 --> 0:21:16.480
<v Speaker 3>and for that we needed some big Mars quakes, and

0:21:16.520 --> 0:21:18.600
<v Speaker 3>they really didn't happen for the first few years, and

0:21:18.640 --> 0:21:21.160
<v Speaker 3>then right near when the mission was about to end,

0:21:21.240 --> 0:21:23.360
<v Speaker 3>we suddenly had a few. So that was really amazing

0:21:23.400 --> 0:21:25.160
<v Speaker 3>to get that data at the end. So Mars kind

0:21:25.160 --> 0:21:27.560
<v Speaker 3>of kept us hoping for a while and then finally delivered.

0:21:27.800 --> 0:21:30.280
<v Speaker 1>And before you landed on Mars with this seismometer, did

0:21:30.320 --> 0:21:33.560
<v Speaker 1>you have much reason to expect that there were Mars quakes?

0:21:33.720 --> 0:21:36.000
<v Speaker 1>Or it could be that Mars was totally silent.

0:21:36.160 --> 0:21:37.760
<v Speaker 3>I mean it could have been we didn't have any

0:21:37.800 --> 0:21:40.720
<v Speaker 3>direct evidence from Mars quakes. But my geologist friends who

0:21:40.760 --> 0:21:43.399
<v Speaker 3>are used to looking at say tectonic features on the surface,

0:21:43.440 --> 0:21:45.560
<v Speaker 3>looking at things like where are the cracks in the surface,

0:21:45.560 --> 0:21:47.560
<v Speaker 3>where are the mountains, they would have told me to

0:21:47.600 --> 0:21:52.040
<v Speaker 3>expect Mars quakes because they see movements geologically, they see

0:21:52.080 --> 0:21:55.040
<v Speaker 3>movements on the surface. But also, luckily, we kind of

0:21:55.040 --> 0:21:57.720
<v Speaker 3>have our own source of Mars quakes. In a way,

0:21:58.040 --> 0:22:02.120
<v Speaker 3>when meteors hit planet, they crash into them. They're kind

0:22:02.160 --> 0:22:05.400
<v Speaker 3>of like a hammer that's smashing into a bell, right,

0:22:05.600 --> 0:22:07.600
<v Speaker 3>And so a lot of the Mars quakes we measured

0:22:07.640 --> 0:22:10.119
<v Speaker 3>were actually caused by meteors that hit Mars as opposed

0:22:10.160 --> 0:22:12.520
<v Speaker 3>to just tectonic activity happening in the interior.

0:22:12.600 --> 0:22:14.800
<v Speaker 1>Well, it's terrifying to me or feel a little conflicted

0:22:14.960 --> 0:22:18.359
<v Speaker 1>the geologists are rooting for quakes and rooting for like

0:22:18.400 --> 0:22:20.880
<v Speaker 1>big impacts because they're like, ooh, yay data.

0:22:21.760 --> 0:22:23.200
<v Speaker 2>Yes exactly, I will.

0:22:23.280 --> 0:22:25.719
<v Speaker 3>I mean, as a funny story on the mission, we

0:22:25.880 --> 0:22:27.879
<v Speaker 3>did at one point, so the Insight mission was on

0:22:27.920 --> 0:22:32.280
<v Speaker 3>the surface when the Perseverance rover was planning to land,

0:22:32.520 --> 0:22:34.760
<v Speaker 3>and we did kind of do a calculation where if

0:22:34.760 --> 0:22:37.840
<v Speaker 3>the landing didn't go so well would be able to

0:22:37.880 --> 0:22:39.000
<v Speaker 3>detect the way from that.

0:22:39.160 --> 0:22:42.080
<v Speaker 2>Luckily that didn't happen. We had a very nice landing.

0:22:42.520 --> 0:22:45.119
<v Speaker 1>Congratulations on your landing. Too bad we didn't get some

0:22:45.119 --> 0:22:48.600
<v Speaker 1>cool data though from your explosion of your huge project.

0:22:48.800 --> 0:22:51.159
<v Speaker 1>Oh my gosh. All right, this is really fun and

0:22:51.200 --> 0:22:53.240
<v Speaker 1>I want to hear a lot more about what's going

0:22:53.280 --> 0:23:09.639
<v Speaker 1>on inside our planet. But first let's take a quick break. Okay,

0:23:09.640 --> 0:23:12.600
<v Speaker 1>we're back. We're talking to Professor Sabina Stanley, author of

0:23:12.640 --> 0:23:16.959
<v Speaker 1>the book What's Hidden Inside Planets, about what's inside our planet.

0:23:17.240 --> 0:23:20.399
<v Speaker 1>You mentioned earlier that it was amazing that insight worked.

0:23:20.520 --> 0:23:22.399
<v Speaker 1>Is that just because it's hard to land stuff on

0:23:22.560 --> 0:23:25.159
<v Speaker 1>Mars and operate a robot on another planet or was

0:23:25.200 --> 0:23:28.959
<v Speaker 1>there something particularly challenging about a seismometer on another planet.

0:23:29.119 --> 0:23:32.080
<v Speaker 3>Yeah, Inside had a lot of firsts, I would say, right,

0:23:32.119 --> 0:23:34.359
<v Speaker 3>it wasn't the first lander. We've had other landers on

0:23:34.359 --> 0:23:36.080
<v Speaker 3>the surface, but this was the first time we were

0:23:36.119 --> 0:23:38.560
<v Speaker 3>going to take equipment that was stored on top of

0:23:38.600 --> 0:23:41.320
<v Speaker 3>the lander and actually physically move it to put it

0:23:41.359 --> 0:23:43.280
<v Speaker 3>on the surface. So there were lots of ways that

0:23:43.320 --> 0:23:45.640
<v Speaker 3>could have gone wrong. Right, This lander had this arm

0:23:46.080 --> 0:23:48.800
<v Speaker 3>type device that had to pick up the seismometer on

0:23:48.920 --> 0:23:52.960
<v Speaker 3>the lander and move it onto the surface. So that required,

0:23:53.119 --> 0:23:54.760
<v Speaker 3>you know, tons of work to get that to just

0:23:54.840 --> 0:23:57.439
<v Speaker 3>work properly. Then it had to put a windshield on

0:23:57.520 --> 0:23:59.920
<v Speaker 3>top of the seismometer to make sure that we didn't

0:24:00.000 --> 0:24:03.120
<v Speaker 3>measure a bunch of wind basically because wind also shakes schismometers.

0:24:03.960 --> 0:24:06.760
<v Speaker 3>Then you know that the seismometer wasn't the only instrument

0:24:07.080 --> 0:24:11.560
<v Speaker 3>on Insight. There was also a thermal probe what we

0:24:11.800 --> 0:24:14.639
<v Speaker 3>called the mole, which was supposed to dig down about

0:24:14.680 --> 0:24:18.440
<v Speaker 3>ten meters and take temperature measurements at depth, which would

0:24:18.560 --> 0:24:21.320
<v Speaker 3>have told us about the heat flow coming out of Mars.

0:24:21.600 --> 0:24:23.240
<v Speaker 2>Again, this was going to be the first time.

0:24:23.040 --> 0:24:27.879
<v Speaker 3>Anything like this was tried, and unfortunately we couldn't get

0:24:27.880 --> 0:24:30.960
<v Speaker 3>the mole to dig deeper than about tens of centimeters.

0:24:31.240 --> 0:24:35.399
<v Speaker 3>The properties of the soils kind of a word we use,

0:24:35.440 --> 0:24:38.840
<v Speaker 3>but the properties of the sand on Mars were not

0:24:38.960 --> 0:24:42.640
<v Speaker 3>as we expected, and just the device couldn't actually use

0:24:42.680 --> 0:24:45.159
<v Speaker 3>friction to dig down deeper and deeper. So that was

0:24:45.200 --> 0:24:48.840
<v Speaker 3>a struggle and we actually the Insight engineering team that

0:24:49.280 --> 0:24:51.040
<v Speaker 3>worked on this and the scientists that worked on this,

0:24:51.240 --> 0:24:52.720
<v Speaker 3>you know, I wasn't part of this. It was just

0:24:52.760 --> 0:24:55.479
<v Speaker 3>amazing the things that they tried, and in the end

0:24:55.480 --> 0:24:57.199
<v Speaker 3>we actually did get some good science out of it.

0:24:57.200 --> 0:24:58.720
<v Speaker 2>We measured more sort of the thermal.

0:24:58.440 --> 0:25:00.600
<v Speaker 3>Properties at the upper part of the cross as opposed

0:25:00.640 --> 0:25:03.359
<v Speaker 3>to deeper down. But it was just amazing to see

0:25:03.560 --> 0:25:05.919
<v Speaker 3>how much they tried to work on doing this first

0:25:06.040 --> 0:25:07.960
<v Speaker 3>digging on here. You know, we talked about digging on

0:25:08.000 --> 0:25:10.560
<v Speaker 3>the Earth is hard. Now imagine digging on another planet

0:25:10.560 --> 0:25:12.399
<v Speaker 3>without humans, and it's even harder.

0:25:12.600 --> 0:25:15.000
<v Speaker 1>Wonderful, And then what are the plans for the future.

0:25:15.080 --> 0:25:18.120
<v Speaker 1>Is NASA planning to dig into the surfaces of any

0:25:18.160 --> 0:25:21.520
<v Speaker 1>other objects in the Solar System or put seismometers on

0:25:21.560 --> 0:25:22.520
<v Speaker 1>any other surfaces.

0:25:22.680 --> 0:25:25.800
<v Speaker 3>So I think seismometers is definitely something that's going to go.

0:25:25.960 --> 0:25:28.040
<v Speaker 3>So there is a big push right now to send

0:25:28.080 --> 0:25:31.000
<v Speaker 3>spacecraft back to the Moon so that we can better

0:25:31.119 --> 0:25:35.320
<v Speaker 3>understand our closest celestial body, let's say. And so there

0:25:35.359 --> 0:25:37.840
<v Speaker 3>is a mission that will involve putting a seismometer, putting

0:25:37.840 --> 0:25:40.240
<v Speaker 3>more seismometers on the Moon. We already have some seismometers

0:25:40.280 --> 0:25:42.359
<v Speaker 3>on the Moon that were turned off a while ago

0:25:42.400 --> 0:25:45.400
<v Speaker 3>for budgetary reasons, right, So it'll be great to get

0:25:45.440 --> 0:25:47.960
<v Speaker 3>seismology again on the Moon. But for me, the most

0:25:48.000 --> 0:25:51.920
<v Speaker 3>exciting is that an upcoming mission that's planned to go

0:25:52.000 --> 0:25:55.000
<v Speaker 3>to Titan, which is a moon of Saturn, is actually

0:25:55.000 --> 0:25:56.720
<v Speaker 3>going to have a seismometer on it as well. So

0:25:56.800 --> 0:25:59.000
<v Speaker 3>it'll be interesting to see what we can learn about

0:25:59.000 --> 0:26:00.399
<v Speaker 3>the interior of.

0:26:00.280 --> 0:26:02.240
<v Speaker 1>Titan, and what do we know right now about the

0:26:02.240 --> 0:26:04.960
<v Speaker 1>interior of Titan, And how could we know anything about

0:26:05.000 --> 0:26:07.199
<v Speaker 1>it just from like looking at a few photons that

0:26:07.240 --> 0:26:08.320
<v Speaker 1>happened to reflect off of it.

0:26:08.520 --> 0:26:10.800
<v Speaker 3>So Titan is one of my favorite places, so it's

0:26:10.840 --> 0:26:12.400
<v Speaker 3>really exciting to think about what they're going to see.

0:26:12.400 --> 0:26:14.399
<v Speaker 3>So Titan's a unique place. First of all, it's the

0:26:14.440 --> 0:26:17.440
<v Speaker 3>only other planetary body in the Solar System that has

0:26:17.440 --> 0:26:20.640
<v Speaker 3>a nitrogen based atmosphere that's thick like the Earth's right,

0:26:20.680 --> 0:26:24.560
<v Speaker 3>So earth Is atmosphere is mostly nitrogen, and the surface

0:26:24.560 --> 0:26:27.040
<v Speaker 3>pressure on Titan is about one and a half bars,

0:26:27.080 --> 0:26:29.160
<v Speaker 3>so one and a half Earth atmospheres. But the cool

0:26:29.160 --> 0:26:31.800
<v Speaker 3>thing about Titan is that it's a small planet and

0:26:31.840 --> 0:26:33.719
<v Speaker 3>so it has very little mass and so its gravity

0:26:33.800 --> 0:26:36.159
<v Speaker 3>is really low. So if you were to go to

0:26:36.200 --> 0:26:39.159
<v Speaker 3>Titan and put some cardboard on your arms and flap them,

0:26:39.200 --> 0:26:41.159
<v Speaker 3>you would be able to fly on Titan because you

0:26:41.160 --> 0:26:45.440
<v Speaker 3>have ideal buoyancy situation there. You've got thick atmosphere, low gravity,

0:26:45.480 --> 0:26:47.000
<v Speaker 3>so it's really easy to fly there.

0:26:47.160 --> 0:26:49.560
<v Speaker 1>So in contrast, like they had the helicopter on Mars,

0:26:49.640 --> 0:26:51.680
<v Speaker 1>that was a real challenge because the atmosphere was thin

0:26:52.240 --> 0:26:55.560
<v Speaker 1>and the helicopter needs atmosphere exactly exactly.

0:26:56.080 --> 0:26:59.040
<v Speaker 3>So the Dragonfly mission, which is going to Titan, should

0:26:59.040 --> 0:27:02.040
<v Speaker 3>get there in the mid twenty thirties. It is going

0:27:02.119 --> 0:27:04.920
<v Speaker 3>to involve a dual quad copter. So this thing has

0:27:04.960 --> 0:27:09.520
<v Speaker 3>basically eight rotors and this to me, because I'm Canadian,

0:27:09.600 --> 0:27:12.000
<v Speaker 3>it looks like a skidoo or a snowmobile because it

0:27:12.040 --> 0:27:16.080
<v Speaker 3>has these sled tracks underneath it. But it's basically going

0:27:16.119 --> 0:27:18.880
<v Speaker 3>to fly around land somewhere, do a bunch of science,

0:27:19.200 --> 0:27:22.880
<v Speaker 3>then take off again, look for a new location, scout somewhat,

0:27:23.000 --> 0:27:24.840
<v Speaker 3>then fly to a new location, land again. And so

0:27:24.880 --> 0:27:28.200
<v Speaker 3>it's going to be able to do ground local science

0:27:28.320 --> 0:27:30.760
<v Speaker 3>right at an individual location for a bunch of locations

0:27:30.800 --> 0:27:33.680
<v Speaker 3>over the surface. And that's really the challenge in planetary

0:27:33.720 --> 0:27:36.680
<v Speaker 3>science is this kind of combination of get lots of

0:27:36.760 --> 0:27:39.960
<v Speaker 3>data from lots of different places really locally, really close

0:27:39.960 --> 0:27:41.280
<v Speaker 3>to the surface. So that's going to be a very

0:27:41.320 --> 0:27:42.040
<v Speaker 3>exciting mission.

0:27:42.200 --> 0:27:43.840
<v Speaker 1>We'd have to ask you about that. Is that going

0:27:43.920 --> 0:27:45.960
<v Speaker 1>to be self directed? Is it going to decide on

0:27:46.000 --> 0:27:47.440
<v Speaker 1>its own where to go or is it going to

0:27:47.640 --> 0:27:50.639
<v Speaker 1>wait for signals for minutes and minutes from Earth?

0:27:50.840 --> 0:27:53.639
<v Speaker 3>Full disclosure here, I have no involvement in the Dragonfly mission.

0:27:53.640 --> 0:27:56.320
<v Speaker 3>I'm just a super fan. But my understanding is what

0:27:56.359 --> 0:27:58.720
<v Speaker 3>it's going to do is when it kind of goes

0:27:58.880 --> 0:27:59.880
<v Speaker 3>up the one time.

0:28:00.000 --> 0:28:01.119
<v Speaker 2>When it flies up one time.

0:28:00.960 --> 0:28:03.320
<v Speaker 3>It's going to survey, It's going to look around, then

0:28:03.359 --> 0:28:06.680
<v Speaker 3>it'll come back down recharge its batteries. And during that time,

0:28:06.720 --> 0:28:08.439
<v Speaker 3>when the data gets back to Earth, people are going

0:28:08.520 --> 0:28:11.080
<v Speaker 3>to look around and say, let's go here, right that

0:28:11.160 --> 0:28:13.040
<v Speaker 3>place over there looks kind of interesting. So it'll be

0:28:13.080 --> 0:28:16.159
<v Speaker 3>a combination. Some of the in time flight stuff is

0:28:16.200 --> 0:28:19.159
<v Speaker 3>going to have to be done by the spacecraft by itself,

0:28:19.160 --> 0:28:21.080
<v Speaker 3>but when it comes to making decisions about where to

0:28:21.119 --> 0:28:23.280
<v Speaker 3>go next in terms of big steps, that's going to

0:28:23.320 --> 0:28:24.280
<v Speaker 3>be done by the people.

0:28:24.040 --> 0:28:24.640
<v Speaker 2>Back here on Earth.

0:28:24.680 --> 0:28:27.920
<v Speaker 1>I really liked your comment about needing to sample several places.

0:28:28.200 --> 0:28:30.320
<v Speaker 1>It seems obvious that if you only land on Earth

0:28:30.320 --> 0:28:32.720
<v Speaker 1>in one place, you might conclude, oh, this whole place

0:28:32.800 --> 0:28:35.800
<v Speaker 1>is granted or oh, look, it's all beautiful marble or something.

0:28:36.000 --> 0:28:38.800
<v Speaker 1>Obviously you need to look around to get a better sample.

0:28:39.160 --> 0:28:40.960
<v Speaker 1>And so when we only land on one place on

0:28:41.000 --> 0:28:43.680
<v Speaker 1>the Moon, like the Apollo astronauts, you know, only looked

0:28:43.880 --> 0:28:46.720
<v Speaker 1>or near where they landed, we may have gotten a

0:28:46.720 --> 0:28:49.120
<v Speaker 1>bias sample of what's going on up there. So that's

0:28:49.200 --> 0:28:51.400
<v Speaker 1>really cool that they're going to explore it. So other

0:28:51.480 --> 0:28:53.520
<v Speaker 1>than landing on the surface. In your book, you were

0:28:53.560 --> 0:28:56.960
<v Speaker 1>talking about seeing what's inside a planet by basically how

0:28:56.960 --> 0:28:59.280
<v Speaker 1>it wobbles. Can you walk us through the physics of that,

0:28:59.320 --> 0:29:01.720
<v Speaker 1>the moment off and how it gives us a picture

0:29:01.720 --> 0:29:02.680
<v Speaker 1>of what's inside.

0:29:02.880 --> 0:29:03.200
<v Speaker 2>Yeah.

0:29:03.240 --> 0:29:07.360
<v Speaker 3>Absolutely, So all of the planets spin to some amount, right,

0:29:07.360 --> 0:29:09.400
<v Speaker 3>That's why we have a day on the Earth. And

0:29:10.680 --> 0:29:14.360
<v Speaker 3>when it spins, a planet doesn't just stay a perfect sphere.

0:29:14.360 --> 0:29:16.560
<v Speaker 3>It kind of gets fatter at the equator than it

0:29:16.560 --> 0:29:18.800
<v Speaker 3>does at the poles. Now, it turns out that how

0:29:18.880 --> 0:29:21.360
<v Speaker 3>fat it gets at the equator versus the poles is

0:29:21.400 --> 0:29:24.720
<v Speaker 3>directly related to what the material properties of the object are. So,

0:29:24.760 --> 0:29:26.600
<v Speaker 3>for example, if you had a perfect water planet, right,

0:29:26.680 --> 0:29:28.600
<v Speaker 3>imagine the small planet made of water and you spun

0:29:28.640 --> 0:29:31.720
<v Speaker 3>it there's a specific like ellipsoidal shape you would get

0:29:31.840 --> 0:29:34.560
<v Speaker 3>for a liquid planet, Whereas if you had a dense

0:29:34.640 --> 0:29:37.560
<v Speaker 3>core inside the planet and with a solid layer and

0:29:37.600 --> 0:29:39.800
<v Speaker 3>then a water ocean on the outside, you're going to

0:29:39.800 --> 0:29:42.480
<v Speaker 3>get a different amount of flattening or a different amount

0:29:42.520 --> 0:29:44.960
<v Speaker 3>of kind of bulging at the equator from that. So

0:29:45.000 --> 0:29:47.400
<v Speaker 3>we can actually use the amount of bulging of these

0:29:47.440 --> 0:29:52.000
<v Speaker 3>planets when they're spinning to get information about what's inside.

0:29:52.160 --> 0:29:54.880
<v Speaker 1>So, for example, you spin a basketball, it stays a sphere,

0:29:54.920 --> 0:29:57.160
<v Speaker 1>but if you spin a blog a pizza dough, it

0:29:57.200 --> 0:29:59.840
<v Speaker 1>becomes a disc, right, and so it tells you pizza

0:29:59.840 --> 0:30:02.560
<v Speaker 1>do softer than basketballs. I guess we already knew that,

0:30:02.640 --> 0:30:04.720
<v Speaker 1>But you're saying we can apply the same thing to planets.

0:30:04.920 --> 0:30:07.440
<v Speaker 1>By the deformation of the sphere, we can tell basically

0:30:07.520 --> 0:30:08.480
<v Speaker 1>how rigid it is.

0:30:08.600 --> 0:30:11.200
<v Speaker 3>Yes, absolutely, and also where the dense, how dense it

0:30:11.280 --> 0:30:15.600
<v Speaker 3>is essentially in different parts. So for example, Saturn, Saturn

0:30:15.680 --> 0:30:18.080
<v Speaker 3>is the bulgiest of all the planets in our solar systems.

0:30:18.120 --> 0:30:19.760
<v Speaker 3>Even if if you look at through a telescope, it

0:30:19.760 --> 0:30:22.520
<v Speaker 3>doesn't look like a sphere, It actually looks like more

0:30:22.520 --> 0:30:25.640
<v Speaker 3>of an oblate spheroid. So it's really interesting to look

0:30:25.640 --> 0:30:26.800
<v Speaker 3>at Saturn through a telescope.

0:30:26.920 --> 0:30:29.440
<v Speaker 1>You mean Saturn looks like squished, like somebody sat on it.

0:30:29.560 --> 0:30:31.520
<v Speaker 2>Yes, Saturn looks like someone satur on it.

0:30:31.440 --> 0:30:34.880
<v Speaker 1>In the best possible way. I mean Saturn's beautiful, Yes, yes, absolutely.

0:30:35.160 --> 0:30:37.680
<v Speaker 3>But because of that, we know that Saturn isn't just

0:30:37.880 --> 0:30:40.080
<v Speaker 3>a ball of hydrogen helium. We know that there have

0:30:40.160 --> 0:30:43.479
<v Speaker 3>to be some rocks inside kind of condensed at the center,

0:30:43.640 --> 0:30:45.920
<v Speaker 3>and then the gas sphere is kind of more on

0:30:45.960 --> 0:30:47.640
<v Speaker 3>the outside of it. So we've actually been able to

0:30:47.640 --> 0:30:50.520
<v Speaker 3>figure that out from the size of its equatorial bulge.

0:30:50.640 --> 0:30:52.560
<v Speaker 2>So that's the first way we can use rotation. There

0:30:52.560 --> 0:30:53.160
<v Speaker 2>are other ways.

0:30:53.160 --> 0:30:57.080
<v Speaker 3>So for example, as planets orbit and rotate, they can

0:30:57.400 --> 0:31:00.760
<v Speaker 3>actually as they're rotating, they don't always point their north

0:31:00.800 --> 0:31:04.320
<v Speaker 3>pole to exactly the same location, so they can actually process,

0:31:04.400 --> 0:31:07.840
<v Speaker 3>so their rotational axis can move around in a circle

0:31:08.160 --> 0:31:10.520
<v Speaker 3>about their orbit axis. And if you've ever played with

0:31:10.600 --> 0:31:12.960
<v Speaker 3>like a top, like a toy top, and you've spun

0:31:13.000 --> 0:31:15.760
<v Speaker 3>it and you've seen it make this little wobbly circlar pattern,

0:31:15.840 --> 0:31:18.800
<v Speaker 3>planets do the same thing. So planetary rotation axis wobble,

0:31:18.880 --> 0:31:21.040
<v Speaker 3>they process, and they also do this thing called nutating

0:31:21.120 --> 0:31:24.000
<v Speaker 3>where they kind of dip down a little bit, and

0:31:24.200 --> 0:31:28.000
<v Speaker 3>the period of those procession motions and the kind of

0:31:28.040 --> 0:31:31.760
<v Speaker 3>how cyclical they are really tells us about the interior

0:31:31.800 --> 0:31:32.600
<v Speaker 3>properties as well.

0:31:32.680 --> 0:31:34.280
<v Speaker 1>But why does it happen in the first place, I mean,

0:31:34.400 --> 0:31:37.360
<v Speaker 1>does an angular momentum tell us that it should we

0:31:37.360 --> 0:31:39.760
<v Speaker 1>spin along the same axis? Is this the effect of

0:31:39.840 --> 0:31:41.400
<v Speaker 1>like other things pulling on it?

0:31:41.640 --> 0:31:42.440
<v Speaker 2>Yes, exactly.

0:31:42.560 --> 0:31:45.160
<v Speaker 3>So if Earth were alone, if it was just the Earth,

0:31:45.160 --> 0:31:46.920
<v Speaker 3>then nothing else was around, we would not have any

0:31:47.000 --> 0:31:50.920
<v Speaker 3>procession or mutation. But we've got the Sun, we've got

0:31:50.960 --> 0:31:54.400
<v Speaker 3>the Moon nearby, and both of those things causecessional motions

0:31:54.400 --> 0:31:58.000
<v Speaker 3>and wobbling nutational motions that affect our orbit in our day.

0:31:58.200 --> 0:32:00.680
<v Speaker 1>So Jupiter and the other things are pulling on the

0:32:00.720 --> 0:32:03.960
<v Speaker 1>Earth and changing the direction of its spin axis basically

0:32:04.120 --> 0:32:06.960
<v Speaker 1>like where the north pole is pointing in the galaxy.

0:32:07.640 --> 0:32:10.200
<v Speaker 1>And you're saying that tells us something about what's inside

0:32:10.240 --> 0:32:12.280
<v Speaker 1>the Earth. People, I think are used to thinking about

0:32:12.360 --> 0:32:14.440
<v Speaker 1>the gravitational model of like, well, you can treat the

0:32:14.440 --> 0:32:16.960
<v Speaker 1>whole planet as a point mass at its center of mass,

0:32:17.160 --> 0:32:19.000
<v Speaker 1>you can't learn anything else about it. So how is

0:32:19.040 --> 0:32:21.600
<v Speaker 1>it possible to know something about the distribution of mass

0:32:21.640 --> 0:32:24.280
<v Speaker 1>inside the planet from how it's spin wobbles.

0:32:24.440 --> 0:32:26.960
<v Speaker 3>So the wobbling and the spin can tell you things,

0:32:27.000 --> 0:32:29.080
<v Speaker 3>for example, like if you have a liquid layer inside

0:32:29.080 --> 0:32:30.920
<v Speaker 3>the planet. So I don't know if you've ever played

0:32:30.920 --> 0:32:33.480
<v Speaker 3>this game, but if you take a beach ball and

0:32:33.520 --> 0:32:35.960
<v Speaker 3>you put like a little pocket of water in it

0:32:36.040 --> 0:32:37.680
<v Speaker 3>and you try to throw it to someone, it moves

0:32:37.720 --> 0:32:40.800
<v Speaker 3>completely differently than if you don't. Or even easier, take

0:32:40.840 --> 0:32:44.360
<v Speaker 3>an egg. Take a raw egg and take a cooked egg,

0:32:44.520 --> 0:32:47.200
<v Speaker 3>both still in their shells, and put them on your counter.

0:32:47.000 --> 0:32:49.280
<v Speaker 2>And spin them, and you will see that they spin.

0:32:49.280 --> 0:32:51.760
<v Speaker 3>Very differently because one of them has liquids inside of

0:32:51.760 --> 0:32:54.040
<v Speaker 3>it and the other one is fully solid. So we

0:32:54.080 --> 0:32:58.040
<v Speaker 3>can use the way that the spin axis wobbles to

0:32:58.080 --> 0:33:00.000
<v Speaker 3>figure out where are there liquid layers in this place?

0:33:00.320 --> 0:33:02.880
<v Speaker 2>Is it fully solid that sort of thing I see?

0:33:03.320 --> 0:33:05.600
<v Speaker 1>Is this planet more like a soft or hard boiled egg.

0:33:06.880 --> 0:33:10.120
<v Speaker 1>That's incredible, And can't you also measure the moment of

0:33:10.120 --> 0:33:12.520
<v Speaker 1>inertia of the planet and tell like where the mass

0:33:12.560 --> 0:33:15.080
<v Speaker 1>is distributed, Like you can tell the difference between like

0:33:15.160 --> 0:33:17.360
<v Speaker 1>all the mass being at the core versus all the

0:33:17.400 --> 0:33:18.680
<v Speaker 1>mass being at the surface.

0:33:19.040 --> 0:33:21.200
<v Speaker 3>Yeah, so it's a bit complicated in the math, but

0:33:21.240 --> 0:33:23.880
<v Speaker 3>it turns out that the precession rate, so how fast

0:33:24.280 --> 0:33:27.920
<v Speaker 3>the axis of the rotation processes about the orbit normal.

0:33:27.960 --> 0:33:28.800
<v Speaker 2>I'll give you any example.

0:33:28.840 --> 0:33:31.040
<v Speaker 3>So on the Earth right now, our north pole points

0:33:31.080 --> 0:33:33.040
<v Speaker 3>to the North Star. It was named lat Way for

0:33:33.080 --> 0:33:35.760
<v Speaker 3>a very specific reason. But it's moving around and in

0:33:35.800 --> 0:33:38.520
<v Speaker 3>about twenty it takes about twenty six thousand years for

0:33:38.640 --> 0:33:41.520
<v Speaker 3>that pole to get back to the North Star. Right,

0:33:41.640 --> 0:33:45.360
<v Speaker 3>So the period of our orbit is twenty six thousand years,

0:33:45.800 --> 0:33:49.760
<v Speaker 3>and that period can be used to actually determine the

0:33:49.800 --> 0:33:53.640
<v Speaker 3>moment of inertia of the Earth through some fancy math formulas.

0:33:53.960 --> 0:33:56.840
<v Speaker 3>And so if we can measure the precession rate or

0:33:56.880 --> 0:33:59.440
<v Speaker 3>the period for other planetary bodies, we can also figure

0:33:59.440 --> 0:34:00.640
<v Speaker 3>out their moment of inertia.

0:34:00.920 --> 0:34:04.120
<v Speaker 1>Wow, twenty six thousand years. How long have we been

0:34:04.160 --> 0:34:06.680
<v Speaker 1>making these measurements? Couldn't have been more than a thousand

0:34:06.800 --> 0:34:07.680
<v Speaker 1>years that maximum?

0:34:07.760 --> 0:34:10.239
<v Speaker 3>Yeah, yeah, it's definitely less than that. But you know,

0:34:10.280 --> 0:34:11.840
<v Speaker 3>you can you can trace out a little arc of

0:34:11.880 --> 0:34:13.640
<v Speaker 3>a circle, then you can pretty much draw out the

0:34:13.680 --> 0:34:14.400
<v Speaker 3>rest of the circle.

0:34:14.600 --> 0:34:16.080
<v Speaker 1>Yeah, I guess we have a model and we can

0:34:16.120 --> 0:34:19.279
<v Speaker 1>fit to that little arc. That's amazing, incredible. We can

0:34:19.360 --> 0:34:22.600
<v Speaker 1>learn so much about what's inside these objects without even

0:34:22.680 --> 0:34:25.160
<v Speaker 1>ever going inside. All right, I can't wait to talk

0:34:25.160 --> 0:34:27.040
<v Speaker 1>about this some more, but first we have to take

0:34:27.160 --> 0:34:42.840
<v Speaker 1>another break. Okay, we're back and we're talking to Professor

0:34:42.880 --> 0:34:46.280
<v Speaker 1>Sabina Stanley, author of the new book What's Hidden Inside

0:34:46.280 --> 0:34:49.600
<v Speaker 1>Planets about what's inside the Earth and other planets. Now,

0:34:49.600 --> 0:34:51.800
<v Speaker 1>I want to talk about sort of how the inside

0:34:51.840 --> 0:34:55.520
<v Speaker 1>affects the outside, because obviously, if you're just curious about

0:34:55.520 --> 0:34:57.200
<v Speaker 1>how the solar system is formed, you want to know,

0:34:57.239 --> 0:35:00.000
<v Speaker 1>like what's inside the Earth. But even if you're not,

0:35:00.239 --> 0:35:03.359
<v Speaker 1>like it has an effect on living on the surface, right,

0:35:03.600 --> 0:35:06.640
<v Speaker 1>tell us about how the magnetic field of these things

0:35:06.680 --> 0:35:09.200
<v Speaker 1>is generated and how it relates to bubbling soup.

0:35:09.480 --> 0:35:12.600
<v Speaker 2>Yeah, so magnetic fields are my favorite topic. Not gonna lie.

0:35:12.840 --> 0:35:14.200
<v Speaker 2>So here's this amazing thing. Right.

0:35:14.239 --> 0:35:16.120
<v Speaker 3>We're on the surface of the Earth, and one of

0:35:16.120 --> 0:35:18.239
<v Speaker 3>the reasons it's such a nice place to live at

0:35:18.239 --> 0:35:21.160
<v Speaker 3>the moment is because we have this beautiful magnetic field

0:35:21.160 --> 0:35:24.480
<v Speaker 3>that completely envelops the Earth. And that magnetic field what

0:35:24.520 --> 0:35:27.040
<v Speaker 3>it does for us is it shields the surface from

0:35:27.120 --> 0:35:29.439
<v Speaker 3>high energy particles that come from the solar wind, which

0:35:29.480 --> 0:35:31.640
<v Speaker 3>come from the Sun and from cosmic rays that come

0:35:31.640 --> 0:35:34.879
<v Speaker 3>from deep space, and those very high energy particles. If

0:35:35.000 --> 0:35:37.120
<v Speaker 3>we didn't have our magnetic field, they would kind of

0:35:37.120 --> 0:35:39.279
<v Speaker 3>blast the surface of the Earth and they would do

0:35:39.360 --> 0:35:41.520
<v Speaker 3>some terrible things. First of all, they would cause high

0:35:41.560 --> 0:35:44.640
<v Speaker 3>radiation environments, so we'd likely have higher rates of cancer,

0:35:44.719 --> 0:35:49.080
<v Speaker 3>for example. But also they cause lots of electrical disturbances.

0:35:49.120 --> 0:35:51.200
<v Speaker 3>And if you think about our power grid, our power

0:35:51.239 --> 0:35:53.680
<v Speaker 3>grid does not like there to be large fluctuations in

0:35:53.800 --> 0:35:54.960
<v Speaker 3>electromagnetic fields.

0:35:55.080 --> 0:35:57.439
<v Speaker 2>That's another thing that is not so good.

0:35:57.640 --> 0:36:02.280
<v Speaker 3>It also tends to these solar winds that bombard planets.

0:36:02.560 --> 0:36:05.600
<v Speaker 3>They can actually erode the atmosphere of a planet, so

0:36:05.640 --> 0:36:07.840
<v Speaker 3>they can take they can basically, you know, it's like

0:36:07.920 --> 0:36:10.040
<v Speaker 3>pointing a hair dryer at the Earth. You're going to

0:36:10.080 --> 0:36:11.719
<v Speaker 3>be able to blow off all the gas from it.

0:36:12.000 --> 0:36:13.799
<v Speaker 3>So there are all these things that the magnetic field

0:36:13.800 --> 0:36:16.840
<v Speaker 3>actually shields us from. But this magnetic field that surrounds

0:36:16.920 --> 0:36:19.960
<v Speaker 3>us is actually created deep inside the Earth in the

0:36:20.000 --> 0:36:24.520
<v Speaker 3>iron core. So iron is great electrical conductor. When you

0:36:24.520 --> 0:36:26.560
<v Speaker 3>have a great electrical conductor, if you can get it

0:36:26.600 --> 0:36:29.560
<v Speaker 3>moving around in the right way, then you can actually

0:36:29.640 --> 0:36:33.239
<v Speaker 3>generate magnetic fields And the best kind of analogy I

0:36:33.239 --> 0:36:34.880
<v Speaker 3>can think of for this is if anyone has a

0:36:34.880 --> 0:36:38.400
<v Speaker 3>home generator or if they have a bike light that

0:36:38.440 --> 0:36:41.360
<v Speaker 3>they can pedal to get going, you're basically converting the

0:36:41.440 --> 0:36:44.800
<v Speaker 3>kinetic energy of that motion into electromagnetic energy.

0:36:44.880 --> 0:36:45.879
<v Speaker 2>So you either you know.

0:36:45.840 --> 0:36:48.960
<v Speaker 3>You're pedaling, causes your bike light causes currents to flow

0:36:49.280 --> 0:36:52.120
<v Speaker 3>that causes your bike light to shine right, or similar

0:36:52.120 --> 0:36:55.160
<v Speaker 3>in your generator. So in the core of the earth,

0:36:55.560 --> 0:36:59.440
<v Speaker 3>convection which occurs because the center is hotter than the

0:36:59.440 --> 0:37:01.520
<v Speaker 3>outer parts of the core, So you kind of have

0:37:01.560 --> 0:37:03.360
<v Speaker 3>bubbling up like like you would if you put a

0:37:03.360 --> 0:37:05.759
<v Speaker 3>pot of soup on the stove, right, you get the

0:37:05.840 --> 0:37:07.759
<v Speaker 3>bottom of the pot is hot, the top of the

0:37:07.760 --> 0:37:11.040
<v Speaker 3>pot is cold, So you get these overturning motions in

0:37:11.080 --> 0:37:14.080
<v Speaker 3>the soup. Same thing happens in the core, and so

0:37:14.160 --> 0:37:17.759
<v Speaker 3>that overturning motions they create magnetic fields and you get

0:37:17.760 --> 0:37:20.399
<v Speaker 3>what called a dynamo. So the dynamo in the center

0:37:20.400 --> 0:37:22.719
<v Speaker 3>of the earth generates this magnetic field that protects us

0:37:22.800 --> 0:37:23.400
<v Speaker 3>on the surface.

0:37:23.600 --> 0:37:27.080
<v Speaker 1>Amazing, And so you're saying that it's the convection cells

0:37:27.280 --> 0:37:30.320
<v Speaker 1>that generate the magnetic field, not for example, the spinning

0:37:30.360 --> 0:37:30.920
<v Speaker 1>of the planet.

0:37:31.320 --> 0:37:36.560
<v Speaker 3>Right, So there's a somewhat common misunderstanding out there that

0:37:36.680 --> 0:37:38.720
<v Speaker 3>the reason that Earth has a magnetic field, for example,

0:37:38.760 --> 0:37:41.560
<v Speaker 3>is due to its spinning. And this has been used sometimes,

0:37:41.560 --> 0:37:45.160
<v Speaker 3>for example, to explain why Venus, which is spinning very slowly,

0:37:45.600 --> 0:37:46.920
<v Speaker 3>doesn't have a magnetic field.

0:37:47.040 --> 0:37:47.880
<v Speaker 2>And it turns out.

0:37:47.719 --> 0:37:50.600
<v Speaker 3>That you don't need spinning at all to generate a

0:37:50.640 --> 0:37:53.800
<v Speaker 3>magnetic field. So magnetic fields can be generated through dynamo

0:37:53.840 --> 0:37:58.800
<v Speaker 3>processes without spinning. Now, spinning sometimes helps in organizing motions

0:37:58.800 --> 0:38:01.200
<v Speaker 3>and stuff like that, but it's not actually a requirement.

0:38:01.400 --> 0:38:03.759
<v Speaker 3>So it's the convective motions, not the spinning, right.

0:38:03.920 --> 0:38:06.400
<v Speaker 1>And so in your analogy, you're talking about like peddling

0:38:06.640 --> 0:38:09.879
<v Speaker 1>your bicycle to generate electricity, And we haven't seen any

0:38:09.920 --> 0:38:12.680
<v Speaker 1>magnetic monopoles in our universe, so we know that to

0:38:12.760 --> 0:38:15.120
<v Speaker 1>generate magnetic fields you have to take a charge and

0:38:15.200 --> 0:38:18.239
<v Speaker 1>put it in motion, which is how electrical generators work.

0:38:18.320 --> 0:38:21.680
<v Speaker 1>But what is the charge here? Like we have flows

0:38:21.719 --> 0:38:24.560
<v Speaker 1>of iron. Iron is obviously metallic and it conducts, but

0:38:24.800 --> 0:38:27.560
<v Speaker 1>don't you need some ion in motion in order to

0:38:27.560 --> 0:38:30.000
<v Speaker 1>get a current going? What generates the actual current? If

0:38:30.040 --> 0:38:32.520
<v Speaker 1>you just have neutral iron how does that generate a

0:38:32.560 --> 0:38:33.280
<v Speaker 1>magnetic field.

0:38:33.480 --> 0:38:36.319
<v Speaker 3>Yeah, it's actually an induction process. So what it is

0:38:36.320 --> 0:38:39.319
<v Speaker 3>is you've got a good electrical conductor and imagine you

0:38:39.400 --> 0:38:42.359
<v Speaker 3>have a magnetic field and it's frozen into a good

0:38:42.360 --> 0:38:46.720
<v Speaker 3>electrical conductor. So magnetic fields tend to stick inside good conductors.

0:38:46.719 --> 0:38:48.600
<v Speaker 2>They don't like to change. But imagine then that.

0:38:48.560 --> 0:38:51.640
<v Speaker 3>You start moving that conductor around relative to itself, so

0:38:51.680 --> 0:38:53.480
<v Speaker 3>you shear it, you pull it apart a little bit.

0:38:53.640 --> 0:38:56.000
<v Speaker 3>That magnetic field has to go with it, so you

0:38:56.080 --> 0:38:59.320
<v Speaker 3>stretch and twist the magnetic fields through the motion itself

0:38:59.560 --> 0:39:01.080
<v Speaker 3>to create new magnetic fields.

0:39:01.160 --> 0:39:05.760
<v Speaker 1>Wow. Fascinating. And the Earth's magnetic field, though it's pretty reliable,

0:39:05.840 --> 0:39:08.200
<v Speaker 1>is not actually constant. Isn't it gradually changing?

0:39:08.400 --> 0:39:08.600
<v Speaker 2>Yes?

0:39:08.680 --> 0:39:12.560
<v Speaker 3>Absolutely, So we have records from the rocks in our crust.

0:39:12.680 --> 0:39:15.440
<v Speaker 3>They can be magnetized at the time that they form,

0:39:15.960 --> 0:39:19.279
<v Speaker 3>and those records tell us that Earth's magnetic field has

0:39:19.360 --> 0:39:21.680
<v Speaker 3>changed over time. We at least have data that shows

0:39:21.719 --> 0:39:24.520
<v Speaker 3>it's been around for about three billion years, if not longer.

0:39:25.360 --> 0:39:27.160
<v Speaker 3>But it hasn't always been the same. So there are

0:39:27.200 --> 0:39:29.160
<v Speaker 3>times in the past where the field has gotten weaker.

0:39:29.200 --> 0:39:31.520
<v Speaker 3>There are times in the past where the field has

0:39:31.600 --> 0:39:34.399
<v Speaker 3>flipped polarity, so the north magnetic pole became the south

0:39:34.480 --> 0:39:38.120
<v Speaker 3>magnetic pole and vice versa. And even today, on like

0:39:38.719 --> 0:39:41.920
<v Speaker 3>weekly time scales, we can measure the small changes in

0:39:41.920 --> 0:39:44.280
<v Speaker 3>the earth magnetic field that are happening from a variety

0:39:44.320 --> 0:39:46.560
<v Speaker 3>of things. Some things are external, but sometimes we can

0:39:46.600 --> 0:39:49.200
<v Speaker 3>also see on a yearly scale we can see the

0:39:49.280 --> 0:39:51.920
<v Speaker 3>changes due to different flows happening in the core of

0:39:51.920 --> 0:39:52.320
<v Speaker 3>the Earth.

0:39:52.520 --> 0:39:54.719
<v Speaker 1>Can we use these changes in the magnetic field to

0:39:54.719 --> 0:39:57.040
<v Speaker 1>sort of image those flows the same way we can

0:39:57.280 --> 0:39:59.640
<v Speaker 1>see changes in the gravitational field to give us a

0:39:59.640 --> 0:40:00.919
<v Speaker 1>picture of what's inside the Earth.

0:40:01.000 --> 0:40:04.000
<v Speaker 3>Yeah, it gets a little more challenging the deeper you go.

0:40:04.200 --> 0:40:06.640
<v Speaker 3>And with magnetic fields, what we can see, for example,

0:40:06.800 --> 0:40:09.040
<v Speaker 3>is because we know it's a good electrical conductor, if

0:40:09.040 --> 0:40:11.520
<v Speaker 3>we see a magnetic field pattern drifting.

0:40:11.120 --> 0:40:11.800
<v Speaker 2>In one direction.

0:40:12.120 --> 0:40:14.360
<v Speaker 3>So for example, there's this kind of famous thing we

0:40:14.400 --> 0:40:17.680
<v Speaker 3>talk about in geomagnetism called the westward drift. So if

0:40:17.719 --> 0:40:19.759
<v Speaker 3>you follow certain features of the magnetic field, you see

0:40:19.760 --> 0:40:22.440
<v Speaker 3>they all kind of drift westward, and we interpret that

0:40:22.480 --> 0:40:25.080
<v Speaker 3>to being there's flow generally in the westward direction.

0:40:25.120 --> 0:40:26.000
<v Speaker 2>There's like a jet.

0:40:25.760 --> 0:40:29.280
<v Speaker 3>Stream in the core of the Earth. That's flowing westward,

0:40:29.800 --> 0:40:31.359
<v Speaker 3>that's taking the magnetic field with us.

0:40:31.400 --> 0:40:34.240
<v Speaker 1>Wow, and so how well do we understand this process?

0:40:34.280 --> 0:40:37.280
<v Speaker 1>Are there still open questions about like why it's flipping

0:40:37.360 --> 0:40:39.320
<v Speaker 1>and why it's changing or is it something that we

0:40:39.440 --> 0:40:40.359
<v Speaker 1>understand pretty well?

0:40:40.520 --> 0:40:44.040
<v Speaker 3>So many open questions. So the amazing thing about this process,

0:40:44.080 --> 0:40:46.840
<v Speaker 3>so fluid dynamics. If you've had any experience with climate

0:40:46.880 --> 0:40:50.200
<v Speaker 3>modeling or trying to study flows that happen in pipes

0:40:50.239 --> 0:40:54.279
<v Speaker 3>and so forth, fluids are really complicated. They can they

0:40:54.320 --> 0:40:58.120
<v Speaker 3>can display turbulence for example, or laminar flows depending on

0:40:58.160 --> 0:41:01.640
<v Speaker 3>what types of you know, what what the situation is like.

0:41:02.320 --> 0:41:03.720
<v Speaker 2>Now, if you add to that.

0:41:04.200 --> 0:41:06.799
<v Speaker 3>Add to fluid dynamics magnetic fields and all the things

0:41:06.800 --> 0:41:09.759
<v Speaker 3>that happen with magnetic fields, you almost get an added complication.

0:41:10.560 --> 0:41:12.239
<v Speaker 3>And so when we try to think about, well, how

0:41:12.280 --> 0:41:14.680
<v Speaker 3>do we study the dynamo process, right, we can't really

0:41:14.719 --> 0:41:18.000
<v Speaker 3>wait thousands of years to watch the real system over time.

0:41:18.000 --> 0:41:20.200
<v Speaker 3>We want to study it faster. So you can either

0:41:20.239 --> 0:41:23.240
<v Speaker 3>do experiments or you can try to write a computer

0:41:23.320 --> 0:41:26.280
<v Speaker 3>model that can mimic what's going on in a core

0:41:26.360 --> 0:41:29.800
<v Speaker 3>when it's generating a magnetic field. Experiments are really hard

0:41:29.960 --> 0:41:33.880
<v Speaker 3>turns out that dynamos they like three things. They like

0:41:34.040 --> 0:41:37.480
<v Speaker 3>really good electrical conductors, they like really fast motions, and

0:41:37.520 --> 0:41:40.520
<v Speaker 3>they like really large length scales. And then you start saying, Okay,

0:41:40.560 --> 0:41:44.520
<v Speaker 3>I'm going to build my giant sphere of a really

0:41:44.520 --> 0:41:46.960
<v Speaker 3>good electrical conductor and then spin it really fast, and

0:41:47.000 --> 0:41:49.880
<v Speaker 3>you just you end up with a huge challenging problem.

0:41:49.880 --> 0:41:52.879
<v Speaker 3>The biggest dynamo experiment out there is the three meter

0:41:53.120 --> 0:41:56.600
<v Speaker 3>Dynamo Sphere in Maryland, and it has yet to generate

0:41:56.760 --> 0:42:00.640
<v Speaker 3>an active dynamo, so that's a challenging problem. We use

0:42:00.640 --> 0:42:04.160
<v Speaker 3>computer simulations to study dynamos inside planets. The problem there

0:42:04.840 --> 0:42:07.880
<v Speaker 3>is that planets, the motions, the scales, and the motions

0:42:07.880 --> 0:42:10.719
<v Speaker 3>are so tiny and so fast that there isn't enough

0:42:10.719 --> 0:42:13.719
<v Speaker 3>computer power on the planet to run a simulation accurately.

0:42:13.960 --> 0:42:15.920
<v Speaker 3>So we have to make a lot of assumptions and

0:42:16.000 --> 0:42:19.880
<v Speaker 3>simplifying type conditions, so we aren't able to fully study

0:42:19.880 --> 0:42:20.720
<v Speaker 3>the system the way.

0:42:20.560 --> 0:42:22.960
<v Speaker 2>We want to. We have to be very nuanced in

0:42:23.000 --> 0:42:23.920
<v Speaker 2>how we study it. Well.

0:42:23.960 --> 0:42:27.160
<v Speaker 1>Do we understand why the Earth's flipping of the magnetic

0:42:27.200 --> 0:42:29.839
<v Speaker 1>field seems so irregular compared to, for example, the Sun,

0:42:29.880 --> 0:42:32.760
<v Speaker 1>which has this rock solid solar cycle of eleven years.

0:42:32.920 --> 0:42:35.560
<v Speaker 3>Yeah, we don't fully understand why at all. We can't

0:42:35.600 --> 0:42:37.799
<v Speaker 3>even kind of predict what we would expect for other

0:42:37.840 --> 0:42:39.680
<v Speaker 3>planets as well. We have what I would call a

0:42:39.719 --> 0:42:42.759
<v Speaker 3>hand way the understanding, and that we would describe the

0:42:42.760 --> 0:42:46.480
<v Speaker 3>core fluid as being a very nonlinear system that can

0:42:46.560 --> 0:42:51.120
<v Speaker 3>have different attractors or different stable systems. And sometimes it's

0:42:51.160 --> 0:42:53.640
<v Speaker 3>in one stable position, sometimes it's another. And so if

0:42:53.640 --> 0:42:55.759
<v Speaker 3>you have something near a stable position, imagine you have

0:42:55.800 --> 0:42:59.480
<v Speaker 3>a ball sitting and you have like a nice valley

0:42:59.480 --> 0:43:01.239
<v Speaker 3>in two hill on the side, and you stick the

0:43:01.280 --> 0:43:03.600
<v Speaker 3>ball on one of the tops of the hills, right,

0:43:03.640 --> 0:43:05.759
<v Speaker 3>it'll pretty much stay there, but maybe if you shake

0:43:05.800 --> 0:43:07.279
<v Speaker 3>it a little bit too much, give it a bit

0:43:07.280 --> 0:43:10.040
<v Speaker 3>too many perturbations, it'll sink down and go to the

0:43:10.040 --> 0:43:13.600
<v Speaker 3>other stable position. So we think that some perturbations in

0:43:13.640 --> 0:43:16.440
<v Speaker 3>the fluid can sometimes cause the field of flip, but

0:43:16.560 --> 0:43:18.360
<v Speaker 3>we don't have a good way to, for example, predict

0:43:18.440 --> 0:43:20.440
<v Speaker 3>when the next flip is going to happen, what's the

0:43:20.719 --> 0:43:23.280
<v Speaker 3>key factor that causes such a flip for example?

0:43:23.280 --> 0:43:24.800
<v Speaker 2>And these are all areas of current research.

0:43:24.920 --> 0:43:29.440
<v Speaker 1>Wow. And then as we discover planets in other solar systems.

0:43:29.719 --> 0:43:33.160
<v Speaker 1>How do we begin to do geology of those planets?

0:43:33.200 --> 0:43:35.520
<v Speaker 1>And first, I guess there's a trivial question is would

0:43:35.560 --> 0:43:37.719
<v Speaker 1>you call it geology? Geology is to study the Earth,

0:43:37.800 --> 0:43:40.120
<v Speaker 1>so it is this like exo planetology, what do you

0:43:40.120 --> 0:43:40.480
<v Speaker 1>call it?

0:43:40.640 --> 0:43:41.880
<v Speaker 2>This is a great question.

0:43:42.000 --> 0:43:44.839
<v Speaker 3>I think the norm has been to refer to geology

0:43:44.920 --> 0:43:46.600
<v Speaker 3>as looking at rocks.

0:43:46.320 --> 0:43:48.480
<v Speaker 2>And it doesn't matter where those rocks are. So rocks.

0:43:48.640 --> 0:43:51.080
<v Speaker 3>There are Mars geologists, I'll just get that out there,

0:43:51.080 --> 0:43:54.800
<v Speaker 3>instead of mars oologists or whatever you would call them instead. Yeah,

0:43:54.800 --> 0:43:58.520
<v Speaker 3>with exoplanets, the challenge there is the type of information

0:43:58.600 --> 0:44:00.920
<v Speaker 3>you can get can be quite limitted compared to what

0:44:00.920 --> 0:44:03.160
<v Speaker 3>we can get when we're in our own Solar system

0:44:03.239 --> 0:44:05.760
<v Speaker 3>or here on the Earth. But even with the standard

0:44:05.760 --> 0:44:09.880
<v Speaker 3>techniques that can discover exoplanets, right, if you think about

0:44:10.080 --> 0:44:13.400
<v Speaker 3>the methods involving radial velocity detection, so where you measure

0:44:13.480 --> 0:44:17.040
<v Speaker 3>fluctuations in the stars light curve caused by the motion

0:44:17.200 --> 0:44:19.400
<v Speaker 3>of a planet around it, you get information about the

0:44:19.400 --> 0:44:21.719
<v Speaker 3>period of the orbit, and that can also give you

0:44:21.960 --> 0:44:24.840
<v Speaker 3>measurements about the mass of the planet. Then if you

0:44:24.960 --> 0:44:27.560
<v Speaker 3>use transit where a planet passes in front of or

0:44:27.560 --> 0:44:30.160
<v Speaker 3>behind a star, you can get information about the size

0:44:30.200 --> 0:44:31.799
<v Speaker 3>of the planet. So as soon as you have the

0:44:31.840 --> 0:44:33.600
<v Speaker 3>size and the mass, you already have kind of an

0:44:33.640 --> 0:44:36.600
<v Speaker 3>average density, a bulk density of the planet. So we

0:44:36.680 --> 0:44:40.080
<v Speaker 3>have sense of whether when we discover these exoplanets, is

0:44:40.120 --> 0:44:43.400
<v Speaker 3>it a gas giant, is it an Earth like planet?

0:44:43.560 --> 0:44:45.799
<v Speaker 3>Is it an ice world like Uranus and Neptune. So

0:44:45.840 --> 0:44:49.600
<v Speaker 3>we can do some very broad geology, let's say, from

0:44:49.640 --> 0:44:52.720
<v Speaker 3>that type of information. But what I'm most excited about

0:44:52.920 --> 0:44:55.279
<v Speaker 3>is the possibilities that are going to come forward with

0:44:55.400 --> 0:44:59.799
<v Speaker 3>JWST because this new telescope is going to be able

0:44:59.840 --> 0:45:04.759
<v Speaker 3>to measure the atmospheres of exoplanets and tell us what

0:45:04.760 --> 0:45:07.440
<v Speaker 3>they're made of. That's going to be crucial information to

0:45:07.480 --> 0:45:10.320
<v Speaker 3>figure out what's actually going on deeper inside the planet.

0:45:10.400 --> 0:45:13.080
<v Speaker 3>Right our atmosphere on Earth is the way it is

0:45:13.160 --> 0:45:15.799
<v Speaker 3>because of interactions with the interior of the Earth, and

0:45:15.880 --> 0:45:17.640
<v Speaker 3>so we're going to be able to use information about

0:45:17.640 --> 0:45:20.120
<v Speaker 3>the atmospheres of these exoplanets to also tell us something

0:45:20.120 --> 0:45:21.040
<v Speaker 3>about the interior.

0:45:21.080 --> 0:45:23.040
<v Speaker 1>What do you mean by that? I know our atmosphere

0:45:23.160 --> 0:45:25.680
<v Speaker 1>is different because we have a magnetic field and because

0:45:25.680 --> 0:45:29.040
<v Speaker 1>of the surface gravity. What else does our atmosphere tell

0:45:29.120 --> 0:45:30.480
<v Speaker 1>us about what's inside the Earth.

0:45:30.640 --> 0:45:33.600
<v Speaker 3>Right, So if there was an alien flying by our

0:45:33.600 --> 0:45:36.080
<v Speaker 3>solar system, and all it could measure is kind of

0:45:36.080 --> 0:45:38.400
<v Speaker 3>the spectrum of our atmosphere, it would be able to

0:45:38.400 --> 0:45:40.200
<v Speaker 3>tell that there was life here most likely.

0:45:40.280 --> 0:45:40.440
<v Speaker 2>Right.

0:45:40.480 --> 0:45:43.120
<v Speaker 3>We've done things to our environment to make it very

0:45:43.200 --> 0:45:46.920
<v Speaker 3>obvious that there is industrial action happening on the surface.

0:45:47.080 --> 0:45:47.279
<v Speaker 2>Right.

0:45:47.360 --> 0:45:50.560
<v Speaker 3>But also, for example, a lot of the processes that

0:45:50.719 --> 0:45:53.840
<v Speaker 3>regulate some of the key species in our atmospheres, like

0:45:53.880 --> 0:45:58.080
<v Speaker 3>carbon dioxide. On Earth, there's the carbon cycle. The carbon

0:45:58.200 --> 0:46:01.360
<v Speaker 3>cycle not only involves the atmosphere, it involves the ocean,

0:46:01.680 --> 0:46:05.440
<v Speaker 3>the surface, and the deep interior. So carbon gets recycled

0:46:05.840 --> 0:46:09.040
<v Speaker 3>inside the Earth, and so we can actually learn about

0:46:09.160 --> 0:46:12.440
<v Speaker 3>how exchanges of materials happen with the interior and the

0:46:12.480 --> 0:46:15.280
<v Speaker 3>atmosphere by looking at how much carbon there is around,

0:46:15.280 --> 0:46:17.360
<v Speaker 3>for example, right. And so the same is true for

0:46:17.480 --> 0:46:20.480
<v Speaker 3>other element cycles, and so the same could be true

0:46:20.480 --> 0:46:21.279
<v Speaker 3>for exoplanets.

0:46:21.400 --> 0:46:24.520
<v Speaker 1>We had Professor Shields on the podcast recently, and she

0:46:24.640 --> 0:46:29.160
<v Speaker 1>does exoplanet climate simulations. We're basically building models of these

0:46:29.200 --> 0:46:31.960
<v Speaker 1>planets and then trying to make them consistent with what

0:46:32.000 --> 0:46:34.799
<v Speaker 1>we might understand from JWST. It sounds like you're talking

0:46:34.840 --> 0:46:37.279
<v Speaker 1>about doing something similar, but you're building models of the

0:46:37.320 --> 0:46:40.480
<v Speaker 1>internals of these planets to explain then the climate in

0:46:40.520 --> 0:46:43.120
<v Speaker 1>the atmosphere, which then tells us about the light we're

0:46:43.120 --> 0:46:45.120
<v Speaker 1>seeing from these planets. So it seems like quite a

0:46:45.120 --> 0:46:48.160
<v Speaker 1>few steps there from the photons we're getting in JWST

0:46:48.520 --> 0:46:51.520
<v Speaker 1>to our model of what's happening inside those planets. Incredible

0:46:51.520 --> 0:46:52.200
<v Speaker 1>that we could learn.

0:46:52.080 --> 0:46:53.640
<v Speaker 2>Anything, Yes, absolutely agree.

0:46:53.800 --> 0:46:56.240
<v Speaker 1>And what about future missions? I know there are space

0:46:56.280 --> 0:46:58.840
<v Speaker 1>telescopes that are going to be looking specifically for planets.

0:46:58.880 --> 0:47:01.000
<v Speaker 1>Are those going to have the toy to tell us

0:47:01.080 --> 0:47:03.319
<v Speaker 1>more about these planets or do we need to wait

0:47:03.400 --> 0:47:07.760
<v Speaker 1>until we can send landers to listen for exoplanet quakes.

0:47:07.840 --> 0:47:12.040
<v Speaker 3>What I'm most excited about for future exoplanet data has

0:47:12.080 --> 0:47:14.239
<v Speaker 3>to do with magnetic fields again, right, So if we

0:47:14.320 --> 0:47:17.640
<v Speaker 3>think Earth having a magnetic field is so important for

0:47:17.719 --> 0:47:20.239
<v Speaker 3>shielding life on the surface, then it might be nice

0:47:20.280 --> 0:47:22.960
<v Speaker 3>if we knew that exoplanets had magnetic fields. It maybe

0:47:22.960 --> 0:47:25.880
<v Speaker 3>it's something we should add to the conditions for a habitable.

0:47:25.520 --> 0:47:26.320
<v Speaker 2>Planet out there.

0:47:26.640 --> 0:47:28.960
<v Speaker 3>And there have been some signs, some evidence that we

0:47:29.040 --> 0:47:31.760
<v Speaker 3>might actually be able to measure magnetic fields of exoplanets

0:47:31.960 --> 0:47:35.600
<v Speaker 3>so there's hope that with even more measurements and so forth,

0:47:35.960 --> 0:47:38.400
<v Speaker 3>we might actually be able to tell in the future

0:47:38.440 --> 0:47:40.440
<v Speaker 3>if an exoplanet has a magnetic field.

0:47:40.200 --> 0:47:42.239
<v Speaker 1>Today, how would that be possible? Are you looking for

0:47:42.320 --> 0:47:45.360
<v Speaker 1>like the Northern lights equivalent on the planet, seeing the

0:47:45.360 --> 0:47:47.319
<v Speaker 1>effect of the magnetic field on the atmosphere.

0:47:47.360 --> 0:47:49.200
<v Speaker 3>So that's one way kind of so it's not the

0:47:49.239 --> 0:47:52.200
<v Speaker 3>Northern lights itself, but actually the way we found out

0:47:52.280 --> 0:47:54.120
<v Speaker 3>Jupiter had a magnetic field. We knew that Jupiter had

0:47:54.120 --> 0:47:56.239
<v Speaker 3>a magnet field in the nineteen sixties even though we'd

0:47:56.239 --> 0:48:00.719
<v Speaker 3>never been there, because electrons that spire roll along the

0:48:00.760 --> 0:48:03.480
<v Speaker 3>magnetic field lines of Jupiter get really close to the

0:48:03.520 --> 0:48:06.080
<v Speaker 3>poles into the atmosphere there right, and that causes aurora

0:48:06.120 --> 0:48:08.800
<v Speaker 3>on Jupiter as well. But it also causes a type

0:48:08.880 --> 0:48:12.040
<v Speaker 3>of radio emissions to come off of Jupiter, and those

0:48:12.160 --> 0:48:14.480
<v Speaker 3>radio emissions get beamed out into space and we could

0:48:14.480 --> 0:48:16.359
<v Speaker 3>actually measure them here on the surface of the Earth.

0:48:16.560 --> 0:48:18.840
<v Speaker 3>So we knew about Jupiter's magnetic field in the nineteen

0:48:18.880 --> 0:48:21.200
<v Speaker 3>sixties before we'd ever gone there, because we received these

0:48:21.280 --> 0:48:25.000
<v Speaker 3>radio emissions. Same is true for any other planet. Now,

0:48:25.000 --> 0:48:27.720
<v Speaker 3>it turns out that the intensity of those radio emissions

0:48:27.760 --> 0:48:30.040
<v Speaker 3>is really important, so you need really strong magnetic fields

0:48:30.040 --> 0:48:31.360
<v Speaker 3>in order to be able to measure them. On the

0:48:31.360 --> 0:48:33.680
<v Speaker 3>surface of the Earth. We have this horrible atmosphere on

0:48:33.719 --> 0:48:35.799
<v Speaker 3>Earth and it blocks a lot of radio emissions, which

0:48:35.840 --> 0:48:38.400
<v Speaker 3>is very frustrating, although kind of good for breathing. So

0:48:38.520 --> 0:48:43.520
<v Speaker 3>I guess, you know, let's say we put a radio

0:48:43.520 --> 0:48:46.120
<v Speaker 3>telescope on the far side of the Moon. That would

0:48:46.120 --> 0:48:49.320
<v Speaker 3>be great for helping to detect radio emissions from exoplanets.

0:48:49.640 --> 0:48:52.319
<v Speaker 3>So there's that method, but they're also what I would

0:48:52.360 --> 0:48:53.560
<v Speaker 3>call sneakier methods.

0:48:53.640 --> 0:48:53.839
<v Speaker 2>Right.

0:48:54.120 --> 0:48:57.880
<v Speaker 3>For example, if you look at the transit spectrum, so

0:48:57.880 --> 0:48:59.600
<v Speaker 3>if you look at a planet that's going in front

0:48:59.600 --> 0:49:03.440
<v Speaker 3>of a sign or a star and you see kind

0:49:03.480 --> 0:49:06.000
<v Speaker 3>of how wide the planet is. People can already kind

0:49:06.000 --> 0:49:08.440
<v Speaker 3>of tell if a planet has an atmosphere by the

0:49:08.480 --> 0:49:11.600
<v Speaker 3>fact that it could have different thicknesses or different radius

0:49:11.640 --> 0:49:14.920
<v Speaker 3>in different wavelengths, and that you know, sometimes the atmosphere

0:49:14.960 --> 0:49:18.239
<v Speaker 3>will let light through, whereas the planet itself won't, right,

0:49:18.320 --> 0:49:20.279
<v Speaker 3>And so that's how we can tell whether something has

0:49:20.320 --> 0:49:23.239
<v Speaker 3>an atmosphere, is what particular wavelengths of light get through

0:49:23.239 --> 0:49:25.560
<v Speaker 3>at different distances. The same can be true about a

0:49:25.560 --> 0:49:28.479
<v Speaker 3>magnetic field. Sometimes a magnetic field can cause certain light

0:49:28.600 --> 0:49:31.279
<v Speaker 3>spectra light frequencies to not get through, so we might

0:49:31.320 --> 0:49:35.480
<v Speaker 3>be actually able to measure a magnetosphere surrounding a planet

0:49:36.160 --> 0:49:39.279
<v Speaker 3>by looking at transit spectra. You can also maybe see

0:49:39.320 --> 0:49:41.960
<v Speaker 3>if a planet has like a tail, right, and so

0:49:42.280 --> 0:49:44.759
<v Speaker 3>sometimes if atmosphere is being blown off a planet, you

0:49:44.840 --> 0:49:46.840
<v Speaker 3>might be able to see that in a transit spectrum

0:49:46.920 --> 0:49:50.080
<v Speaker 3>or through other types of light detection. So there might

0:49:50.080 --> 0:49:52.360
<v Speaker 3>be some sneaky ways to look for magnet fields of

0:49:52.360 --> 0:49:53.279
<v Speaker 3>exoplanets as well.

0:49:53.719 --> 0:49:56.480
<v Speaker 1>Wonderful well, I expect that the next generation of scientists

0:49:56.520 --> 0:49:58.640
<v Speaker 1>will be even more creative about coming up with ways

0:49:58.640 --> 0:50:02.360
<v Speaker 1>to extract a me information from these tiny little blips

0:50:02.360 --> 0:50:03.200
<v Speaker 1>in our telescopes.

0:50:03.360 --> 0:50:04.040
<v Speaker 2>Yes, hopefully so.

0:50:04.280 --> 0:50:06.120
<v Speaker 1>Wonderful well. Thank you very much for coming on the

0:50:06.160 --> 0:50:08.319
<v Speaker 1>podcast and telling us so much about the mysteries that

0:50:08.360 --> 0:50:10.439
<v Speaker 1>are under our feet and the mysteries that are out

0:50:10.440 --> 0:50:11.440
<v Speaker 1>there in the universe.

0:50:11.640 --> 0:50:12.200
<v Speaker 2>Thanks so much.

0:50:12.200 --> 0:50:14.279
<v Speaker 1>This was fun, all right. That was my chat with

0:50:14.320 --> 0:50:17.120
<v Speaker 1>Professor Sabina Stanley again. She's the author of the book

0:50:17.200 --> 0:50:20.520
<v Speaker 1>What's Hidden Inside Plants, which you can get now at

0:50:20.560 --> 0:50:24.120
<v Speaker 1>all reputable booksellers. Thanks very much for listening. Tune in

0:50:24.200 --> 0:50:34.480
<v Speaker 1>next time. Thanks for listening, and remember that Daniel and

0:50:34.560 --> 0:50:37.880
<v Speaker 1>Jorge Explain the Universe is a production of iHeart Radio.

0:50:38.239 --> 0:50:43.319
<v Speaker 1>Or more podcasts from iHeartRadio, visit the iHeartRadio app, Apple Podcasts,

0:50:43.440 --> 0:50:45.800
<v Speaker 1>or wherever you listen to your favorite shows.