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you

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[Music]

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hi okay so I'm not going to talk about

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stars really at all what I want to talk

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about is the sort of the idea that rocky

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planets might have elemental ratios that

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are basically the same as their stars

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but maybe those can be post processed

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through atmospheric escape and so I

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wanted to examine sort of the idea that

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you could lose enough rocky elements

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from the planet's atmosphere to to sort

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of fractioning its actual solid

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abundances so the the idea of

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atmospheric escape from M dwarf planets

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are from really any rocky planets is

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pretty popular in the exit planet

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literature especially this idea that you

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can take a gas giant or a mini Neptune

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and just to rode the entire volatile

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envelope and be left over with a rocky

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planet so I just want to highlight a

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couple of studies here so this is a

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paper from Eric Lopez that was looking

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at the Kepler 36 system and the idea

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that they're exploring is that you have

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a certain amount of rocky material as a

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core and you have of 20% hydrogen or

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helium envelope on top and that the size

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of the rocky core is going to dictate

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how much of that envelope you can Road

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over time so these two planets are

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observed to have they're very close in

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orbital period but they have very

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different observe radii but in his

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models you can take basically the same

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initial envelope abundance and the

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planet with a smaller core you can erode

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all of that envelope whereas the planet

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with a larger core you can only Rhodes

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about 10% of that envelope and then this

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is work from Rodrigo Luthor who we heard

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from earlier looking at also evaporated

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cores this is looking at the level of

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zone for M dwarf planets so this is

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stellar mass and orbital distance in

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this shaded region is the Hubble's own

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of these stars and these contours are

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showing where you have evaporated cores

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so to the left of these lines you have

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planets who have lost their entire

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volatile envelope of about 50% or about

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half of their mass

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as hydrogen so if you have energy

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limited escapes in the planets that

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you're seeing in the handle zone could

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have started off with 50% of their mass

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in hydrogen okay so that's a lot of

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atmosphere that you could lose you can

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play the same game with steam

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atmospheres this is more work from

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Roderigo Luger looking at water loss so

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this is again indoor pool zones and

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looking at the amount of water you can

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lose from a planet due to this extended

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phase and in Dorf evolution where these

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planets are actually in interior to the

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to the initial levels own so the red

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here is just indicating that you have

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lost all of your water your initial

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water envelope I'm and if your stripping

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hydrogen off of of water than you can

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get oxygen build-up so over here they're

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showing the oxygen buildup red is

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basically all of the water has been

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converted into oxygen but over here

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you've actually lost some of your oxygen

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right so you haven't been able to hold

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on to all that oxygen because it's being

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lost along with the hydrogen through

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hydrodynamic drag so if you're losing

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oxygen maybe you can also lose other

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elements as well and this is important

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because magma ocean atmospheres are not

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pure steam and they're not pure hydrogen

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this is work from Bruce vaguely

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published last year looking at the

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compositions of steam atmospheres as a

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function of surface temperature here on

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the x-axis and this is the mole fraction

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of gases in the atmosphere on the y-axis

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so you can see the atmosphere is

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dominated by steam it's got a lot of

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hydrogen but the third most abundant

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hydrogen bearing gas is silicon tetra

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hydroxide at 2000 Kelvin if you go up to

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higher temperatures you get magnesium

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iron sodium hydroxides right so you have

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a reasonably abundant lissa file

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elements in your atmosphere so if you're

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losing hydrogen from the atmosphere then

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you might be dragging these elements

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along for the ride so a lot of this is

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you know based on the idea that you can

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do this and that people have looked at

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this in the solar system for noble gases

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as you can fractionate doe noble gas

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isotope

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through hydrodynamic drag so maybe you

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can do this for rocky elements as well

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and there's at least two ways you can

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fractionate the elements in these

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atmospheres the first is through

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fractional vaporization and then the

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second is is through the dynamical

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effects given that these elements have

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different masses so I'll talk a little

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bit about both of those

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okay so first a fractional vaporization

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is just that the gas composition is not

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the same as the solid material right

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these elements have different

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volatilities and so they're going to go

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into the gas phase at different rates

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depending on the temperature and the

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pressure of your envelope this is

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another figure from Bruce vaguely who

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sort of came up with this idea that you

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could lose silicate elements from from

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these steam atmospheres the X scale here

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is inverse temperature so higher

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temperatures on the left here lower

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temperature on the right and the y-axis

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is the silicon to magnesium ratio in the

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atmosphere and then the two colors here

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are two different pressures so a

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different atmospheric mask basically

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this is lower pressure this is higher

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pressure so what happens is the silicon

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abundance in the atmosphere is very

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strongly pressure dependent but it

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doesn't depend very strongly on

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temperature so as you go up and pressure

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the silicon abundance is going to

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increase in so you're going to increase

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the silicon to magnesium ratio in the

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atmosphere you're also just overall

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increasing the silicon abundance in the

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atmosphere at really high pressures

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silicon tetra hydroxide can actually be

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the second most abundant gas in the

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entire atmosphere so it can make up a

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significant portion magnesium on the

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other hand is not very pressure

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dependent but it is very strongly

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temperature-dependent the abundance of

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magnesium increases as you go to higher

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temperatures and so our silicon and

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magnesium ratio is decreasing over here

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at at high temperatures so if we just

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take this atmosphere and just blow it

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off assume there's no dynamical effects

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at all in order to make a significant

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effect on the rocky body itself you need

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to lose about two weight percent of the

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plan

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it in terms of esteem atmosphere in

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order to lose about 1% of your total

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silicon that's in your mantle and the

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magnesium lost given this you're losing

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a massive atmosphere there's very little

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magnesium in the atmosphere so you're

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actually not losing very much of it so

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then that effect is to decrease the

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silicon magnesium ratio of your mantle

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but what about those dynamical effects

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okay so and that should be that's a

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decided upper limit right so there's no

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dynamical effects in here so what if we

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do take those into account if we're

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looking just at the simple energy

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limited escape we can put a limit on the

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mass of the particles that can be drug

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along with the hydrogen okay so this is

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the crossover mass and basically if the

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mass of your particle is lower than the

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crossover mass then it can escape along

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with the hydrogen then you can convert

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this crossover mass into an effective

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XUV flux so if your planet receives more

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XUV flux than this critical value then

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you can strip off that element from the

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atmosphere an important caveat here is

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of course that the little pile Elmas in

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order to be stripped actually have to be

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in the atmosphere and so that means you

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actually have to be not just in the

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runaway greenhouse effect but you have

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to be in the magma ocean stage where

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you've melted the surface and your

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temperature is at least about 1500

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Kelvin or hotter okay so here I'm

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showing the XUV fluxes of the Hallows

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own planet so these are planets that are

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in the have ozone at five Giga years for

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different stellar masses as a function

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of time this is for a point one solar

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mass star and I'm taking the inner and

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outer habitable zone edges from Ravi

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Cooper operatives work this is a recent

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Venus in the early Mars okay and here's

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a 0.5 solar masses and point nine solar

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masses and here's the runaway greenhouse

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women okay so for the K dwarf here the

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Quinta's don't spend a whole lot of time

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in the runaway greenhouse limit but for

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the in dwarf stars they stay in the

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runaway greenhouse limit for for quite a

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long time

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and then I'm going to compare this xev

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flex that these planets are receiving to

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the critical xev flux for the different

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with a file elements so this depends on

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the atomic masses of hydrogen and MV

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with a file element the planet mass

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which here I'm just taking one earth

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mass and this binary diffusion

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coefficient which is usually measured

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empirically but we don't have those

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measurements for rocky elements so I've

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approached mated them using this that's

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hard spheres formula so here's the

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critical xev flux for silicon for

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magnesium and then for iron you can see

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there's a mass dependence here magnesium

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is the lightest heaviest but these are

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all below the runaway greenhouse limit

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which means that the limiting factor

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here is how long you have a steam

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atmosphere not the the XUV flux that

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you're receiving so if you have a steam

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atmosphere you should be losing these

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elements here's a very preliminary

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calculation for silicon math class I

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haven't really gotten around to the

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other elements yet looking at the

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fraction of silicon that has lost four

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different envelope masses as a function

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of time so starting from one earth ocean

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up to about 400 Earth oceans which for

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reference is about nine weight percent

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of an earth-mass planet so you can see

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this is a log scale down here we have

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very minimal loss of silicon and we only

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really get significant loss of silicon

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up here for about 400 ocean masses so

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this is a very very water rich planet

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and and these curves I should say are

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being cut off where you are reaching a

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surface temperature of about 1400 Kelvin

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so below that the lid to file elements

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drop you might so get a little bit more

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escape but not significant amount so

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just to sum up if you have significant

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envelope stripping of a planet it's

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possible that you could fraction eight

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the little file elements it seems that

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this is only going to be important

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forward very extreme cases of

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of envelope stripping for have alone

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cleanest but it's likely to be much more

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important for planets that are closer to

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the star than they have the ozone I

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didn't really talk about alkali elements

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at all but sodium is both lighter than

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silicon and also more volatile so you

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can imagine that there might be planets

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where you have stripped off most of your

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sodium so next steps we need to look

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also at loss from hydrogen envelopes

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where the volatilities of these elements

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are going to be different gas and mantle

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composition should co-evolve which is

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not happening right now I'm just taking

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a fixed sort of gas composition cloud

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formation might actually hinder this

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kind of loss again for closer in planets

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this is probably not going to matter too

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much but for have ozone planets it could

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could definitely a halt loss and then of

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course there are other loss processes so

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I'll stop there thanks my funding

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sources and take any questions

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Laura this is really cool stuff I was

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curious if you were sort of taking into

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account how much of those ocean masses

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you're losing so could you drive escape

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of those lighter elements and then

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basically at the end you're just

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dragging off silicon because it's

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basically have a silicon atmosphere of

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some kind or silica atmospheres um so

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you mean if so if we have a smaller

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volatile envelope and maybe it's just so

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you really need the water in order to

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get the surface hot enough right to

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vaporize the silicon unless you're much

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closer to the star so you can imagine

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there there are definitely planets like

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55 Cancri E or Colorado 7b or Kepler 10b

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where they're just vaporizing silicon

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without having any kind of atmosphere

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for the the have ozone planets you do

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need some kind of greenhouse warming in

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order to get hot enough to vaporize them

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so at once you lose enough envelope

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you're going to probably condense

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everything back onto the surface yeah