Learn about the science behind the current exploration of the solar system in this free class. Use principles from physics, chemistry, biology, and geology to understand the latest from Mars, comprehend the outer solar system, ponder planets outside our solar system, and search for habitability in our neighborhood and beyond. This course is generally taught at an advanced level assuming a prior knowledge of undergraduate math and physics, but the majority of the concepts and lectures can be understood without these prerequisites. The quizzes and final exam are designed to make you think critically about the material you have learned rather than to simply make you memorize facts. The class is expected to be challenging but rewarding.
Lecture 2.07: Theoretical internal structure
Loading...
Del curso dictado por Caltech
The Science of the Solar System
271 calificaciones
De la lección
Unit 2: The insides of giant planets (week 1)
Conoce a los instructores
Mike BrownProfessor
Planetary Astronomy
Okay, I've been promising that we were going to figure out
what's inside of Jupiter all this time and now we're going to finally do it.
Let's review the last three lectures had a lot of detailed physics in them,
let's just make sure that we remember how those work as a general concept even if
the physics was a little bit much.
First,.
We have the equation of hydrostatic equilibrium.
That equation of hydrostatic equilibrium is the one that tells us
what the pressure is as a function of altitude, which we use z, which is really
just a function of how much mass and force is pushing down on that material.
The other thing that we needed was the equation of state.
The equation of state was critical because it relates.
The pressure, and the density.
It says,
if I have this pressure, this is the density that the material will achieve.
And the equation of state is complicated.
There are experimental methods to figuring them out.
We did one theoretical one where we called,
did this thing called the fair me see, where we had, we found that
pressure was proportional to the density to the 5/3 for very compressed objects.
But that's not the real equation of state of materials.
You really do have to do more complicated calculations and
the calibrate those with experimental data.
We also had the phase diagram.
Phase diagram was critical because for a given pressure and
a temperature it told us the state of the matter.
That is, is the Hydrogen a molecule?
Is it atomic?
Is it ionized?
Or is it that.
Crazy liquid metallic version.
And the last thing we needed to note was something about the heat flow.
We didn't talk much about the heat flow but we now know that there's heat coming
from the inside of Jupiter and that's either being transported from convection.
Maybe from radiation, maybe to little bit from conduction.
We're going to use these four things.
And try to match two simple observations,
the radius of Jupiter and the mass of Jupiter.
Really that's of course the density of Jupiter but
it actual will matter that we're actually doing the radius and total mass.
How do we do that?
Well we start by saying all right here is the upper radius,
we know the radius of Jupiter right here.
And we're going to start with the top layer of material.
We're going to, we know what the temperature is at the very top, so
we know the phase of the material at the very top.
It's an H2.
And we know the energy being dissipated at the very top, that's what we can measure.
We measure the photons coming up, we call this the thing that is the photosphere.
So we start with this very top.
And we slowly add layers.
We add the next layer down, we can figure out the pressure of the next layer down is
because it's just because of the mass of the material pulling down on this.
We know the gravitational field here because we know the total mass of Jupiter
on the inside pulling it down.
We can calculate the pressure, we can calculate the temperature.
If we assume what sort of heat flow that we have in there, we can make sure that
the phase diagram still tells us what the state of matter is and
we calculate a new pressure.
We do the same thing one more time, add another little la-,
layer of mass in through here.
We calculate a new pressure.
We calculate a new temperature.
We check the phase diagram.
We keep on doing the same thing through here.
At some point we'll find the phase diagram and it shows that the.
Hydrogen has turned into metallic hydrogen.
Metallic hydrogen has a different equation of state than molecular hydrogen does, so
we'll have to change to that equation of state.
We keep on going, and when we get to the center of Jupiter right here,
we are either, one of two things is going to happen.
Either it perfectly works, we're finished.
All the mass, if we add up all the mass that we added in through here.
We get the mass of Jupiter or this is what happens in real life if you take
a Hydrogen, Helium composition and you start adding these layers in through here,
you find that you get to the center of Jupiter, you've added all these layers in
through here and you've made a ball that's the same size as Jupiter.
But you have mass leftover on the inside.
What it does that tell you?
That tells you, you cannot make Hydrogen-Helium with the 75% Hydrogen,
25% Helium that we were assuming.
You cannot make something the radius of Jupiter and the mass of Jupiter.
If you want to make something the mass of Jupiter,.
You had to have started at a bigger radius and added the layers
together until you get to the center and you perfectly run out of material.
Now you can imagine starting too big and you add all the layers together and
suddenly you run out of material here and you would have to have a vacuum
in the middle of Jupiter and that makes no sense so
you have to you wou-, you would iterate around, you'd first do this calculation.
Have mass leftover, you would add a little more,
you would do this one say oops that's too much and you would come in the middle and
say I now know for something the mass of Jupiter what the radius has to be
if you're going to make Hydrogen-Helium planet with these ratios.
And for fun, you can do the same thing for any mass that you come up with, here is
mass of Jupiter one in this case and you find that if you take the mass of Jupiter.
You need to have a Hydrogen-Helium ball that's this big,
which is a little bit bigger then the actual size of Jupiter itself.
If you use a little bit less lat mass like, say,
the mass of Saturn, you come up with a ball that's this big.
It gets smaller.
If you use a lot less you come up with something that's this big.
Interestingly if you add more mass than Jupiter, two, three,
four times the mass of Jupiter here.
You get to a maximum and then you start to add more mass and the size goes down.
This is strange behaviour usually you think of if I have a ball of material and
I add more to it it gets bigger, in this case it's the exact opposite and the exact
opposite is because of that quantum mechanical effect that equation of state.
Which is that the additional pressure is so high as you add more mass in through
here that the density increase more than compensates for
the extra material that you have adding on.
And so your objects actually shrink, some think the mass of Jupiter,
made out of hydrogen and helium,
is bigger than something 20 times the mass of Jupiter made out of Hydrogen-Helium.
This is a cool plot seeing how, how hy, Hydrogen-Helium planet would go
as function of mass and it shows once again that Jupiter doesn't fit.
What is going on with Jupiter?
We'll talk also, when we talk about Saturn we'll.
Also, that Saturn doesn't fit either.
What is going on with Saturn?
One or
more of the assumptions that we made in trying to construct Jupiter was wrong.
There was really only one way to make Jupiter smaller for the mass that it is.
And, that's by adding heavier material to it than just Hydrogen and Helium.
Well, that's not a big surprise.
We know that the universe is more than just hydrogen and helium.
But even if we added these small amounts of additional materials that are in, say,
the sun, you would get very little difference.
You might drop it down by a little bit.
Jupiter has to have more material than just Hydrogen and Helium, and
it has to have more of that material than the sun does.
And there are two ways to have that material [INAUDIBLE] there are probably
more then two ways but there are two end members of ways you could have
that material you could imagine that Jupiter just had Hydrogen and
Helium and everything nicely mixed throughout.
Or, you can imagine, that, Jupiter has Hydrogen and Helium and
then a core of solid material that's a different composition.
We'll talk a lot about these two different ideas but I'm going to show you first that
this calculation, this a line that you see right here goes like this,
comes up like that, goes through Jupiter and keeps going.
That a line is for the composition of a planet that's mostly
Hydrogen-Helium except the inside has a core
that is 15 times the mass of the Earth, that's how I'll write Earth mass.
That's a little circle with a plus in it is the Earth symbol.
15 Earth masses.
Of material on the inside.
If I add this 15 Earth-mass core, I can make Jupiter.
Do I have to have a truth 15 Earth-mass core?
No. I can distribute that
material throughout there like this, and
we will use additional observations to try to determine whether or not this 15
Earth-masses that we need, extra, is down here like this or spread throughout.
Now, to be fair, one of the big problems that we have
in constructing our model of Jupiter is that equation of state.
The equation of state, particularly at the highest pressures, is pretty uncertain.
It's uncertain by a factor of a couple, and it's enough uncertain that
you could probably get away with using a slightly different equation of state.
You could probably get away with just Hydrogen and
Helium making it through Jupiter.
Most people think that the equation of state requires that there is this
additional material inside Jupiter, but it's not 100% certain.
What is certain, and again, we'll talk about when we get to Saturn,
this is the symbol for Saturn,.
When we get to Saturn is that even with a modified equation of state,
you can't make Saturn out of just Hydrogen and Helium.
There must be additional ma, material inside of Saturn.
if there's di, additional material inside of Saturn, and we think there probably is
additional material inside of Jupiter, we're going to go on the assumption that
it's, that it's probably really there, in one of these two forms.
And see if we can figure out what might be going on, on the inside.
Explora nuestro catálogo
Inscríbete de manera gratuita y obtén recomendaciones personalizadas, actualizaciones y ofertas.
Coursera brinda acceso universal a la mejor educación del mundo, al asociarse con las mejores universidades y organizaciones, para ofrecer cursos en línea.
© 2018 Coursera Inc. Todos los derechos reservados.
