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hi

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my name is oliver herbert and i'm

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presenting to you today the work on

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atmospheres of rocky accident that i've

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been doing during my phd in snandrus

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so the main one of the main questions of

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astrobiology is whether

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planet itself is dry has no liquid water

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at the surface

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or whether it does have actual water at

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the surface

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so that life as we know it can thrive so

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the big question is how can we actually

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detect this from our own earth

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how can we tell that on other planets

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and therefore

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one has to understand that during for

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example transmission spectroscopy

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one is actually probing the high parts

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of the atmosphere that when the light is

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traveling through the atmosphere

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we actually do see only the composition

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of the high parts of the atmosphere and

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if we are fortunate at some point

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in the future with future

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instrumentations we get some scattering

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effects from

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some particular um cloud condensates and

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those

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we can then um analyze and

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tell which actual condensates that is

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but that is not really

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exactly the crust composition the cross

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condition can be slightly different

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and that is what i am working on and

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what i'm going to present today

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and in order to do so we need to

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understand that

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the crust and the atmosphere there are

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many

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lings for them and especially

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at the very bottom where the crust is

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outgassing into the atmosphere there can

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be volcanism there can be

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plate tectonics which actually drive

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some parts of the er

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from the exposed rock towards the mantle

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again chemical weathering can affect can

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have some effects from the atmosphere

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onto the

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rock composition then higher up in the

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atmosphere

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where we do have potential cloud

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formation the clouds are depleting the

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rest of the uh the elements that are

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used up in the clouds so that the

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element composition below and above the

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clouds are different

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atmospheric loss parts of atmosphere the

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atmosphere can be lost through space

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and then last but definitely not least

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photochemistry stellar radiation cosmic

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rays

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can change the atmospheric composition

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the chemical buildup of the atmosphere

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however

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at the beginning of this talk i would

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only focus on the atmosphere crust

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interaction at the very bottom of this

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atmosphere

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and then provide insights the surface

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conditions and then

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set the preconditions for cloud

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information later in the talk

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the model i'm using is an equilibrium

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chemistry model

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you with an equilibrium conversation

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called gigi chem by peter weitge

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my supervisor and it basically takes a

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given set of elements

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the total element abundances so given

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amount of hydrogen given amount of

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carbon

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nitrogen oxygen but also with elements

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like calcium titanium

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or so and puts them into one big culture

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and they're given pressure given

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temperature

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and then on the basis of minimization of

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gibbs free energy calculates what's most

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stable in the gas phase

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there are no over no supersaturated

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molecules in the gas phase

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and we allow that or we force that by

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actually having condensation and these

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condensates

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are then building up the crust of the

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of the planet that we have so

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one of the big uh components to uh to

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vary here

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is the total element abundance and

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that's what i show you here

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in this plot on the right-hand side

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where we have on the

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on the y-axis the element abundance

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relative to silica and on the x-axis

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um different uh elements and we see when

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we compare the squares and the diamonds

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the ci contract left over up from the

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formation of the solar system which is

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particularly enriched in the volatile

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the gas loving

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um elements like hydrogen carbon

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nitrogen but also sulfur or phosphorus

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in comparison to the bulk silicate earth

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which is earth

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without its core and counting all of the

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elements

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aluminium

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or calcium are very very similar for

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those

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but they have different effects on the

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resulting atmosphere

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and that's what i show you here in this

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plot where i'll walk you through it now

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so it's 100 bar atmosphere and

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temperature range from 100 to 5000

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kelvin

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and on the y-axis we have the molecular

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abundance of the gas species for the

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very high temperatures

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we vaporize the rock we have metal

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oxides dominating the atmosphere

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and then for lower temperatures water

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sulfur

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dioxide and carbon dioxide are the most

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important

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parts of the atmosphere and they then

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condense out at different points

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leaving nitrogen behind for the ci

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contract this image is relatively the

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same

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metal oxides at the high temperature

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range and then

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water carbon dioxide and nitrogen

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leaving behind but there's also methane

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h2co

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and atomic hydrogen and that is called

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because there's just so much more

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volatiles in this model

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if we now want to investigate where the

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hydrogen itself goes where does the

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hydrogen go

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and that's what i show you here in the

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range of thousand two hundred kelvin

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where the water gas is getting low and

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lower in abundance

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and all of the hydrogen is forming soda

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fluoropythology

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those are two phyllosilicates and so uh

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so hydrated rocks

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that actually incorporate oh into the

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lattice structure

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and if we look at the ci chondrite model

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we see that there's a huge variety of

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different phyllosilicates

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that incorporate a lot of the hydrogen

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but there's still enough hydrogen left

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that we can actually form liquid water

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over these

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phyllosilicates that need to be

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saturated we can also

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force our bulk silicate earth model in

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order to

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actually form water and by that we can

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do by increasing hydrogen and oxygen

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abundances

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and then we can saturate the

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phyllosilicates and then on top of that

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we will have

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the liquid water because the phyllis

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liquids are just more much more stable

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so this was only the atmosphere cross

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interaction layer an atmosphere is more

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than that

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and it's also more than just the

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troposphere but for this part

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i'm talking about the troposphere is the

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lower part of the atmosphere where the

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pressure

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over the temperature is just decreasing

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with the pressure

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as shown on the plots here at the bottom

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left here

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and as we build our hydrostatic

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polytropic atmosphere from bottom to top

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we solve chemical phase equilibrium in

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every atmospheric layer

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and every time when there's a condensate

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stable we take the condensate

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take them out interpret them as a

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thermally stable cloud

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and only take the gas phase as the total

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element abundance of the layer above

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and with that we actually do build our

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atmosphere that is actually depleted

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in those condensates that are taken out

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that formed clouds there's no kinetic

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cloud formation in here that's the next

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step to do

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but this is to investigate what is

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thermally stable the fact of this for

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the element for the molecular abundances

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in the atmosphere can be seen in this

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spot on the right hand side

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being the actual molecular abundance

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at the bottom of the atmosphere and then

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going to the left is to the top of the

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atmosphere

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the beginning and especially we see that

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water the blue line and carbon dioxide

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are decreasing significantly throughout

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the atmosphere

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and that is caused by the condensation

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of

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is what actual cloud condensates are

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there water

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the blue lines stable throughout the

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atmosphere and then also graphite at the

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bottom of the atmosphere

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have that ammonium chloride and

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hydrosulfate if you want to investigate

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further uh temperatures at the same time

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of varying the surface

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temperatures that's uh going to be in

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the next spot but it's going to be a bit

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confusing so i'll just

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explain the access here so surface

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temperature

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300 to 1000 kelvin and then yeah each

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atmosphere is one column

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so a model with 400 kelvin starts here

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goes up goes up and it's just one column

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here

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if we plot now all of the condensates in

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here that are thermally stable and

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relatively abundant

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we get this result and that is actually

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really interesting because we

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already see here that we have a

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discrepancy between high temperature

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conditions and low temperature

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condensates

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chloride potassium chloride

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and iron sulfur whereas the low

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temperature condensates are water

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there's carbon the black lines and then

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as i mentioned earlier ammonium chloride

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potassium chloride but also

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sulfur s2 the orange one here forming

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some of the condensates

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if we compare this to the bulk silicate

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earth model

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we see that the overall image is roughly

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the same we have the high temperature

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concept and the low temperature

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condensates

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but there is graphite now breaching this

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gap of high and low temperature

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condensates and actually

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in our models we see that graphics the

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only concept that can do so

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so graphite is quite special and that

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needs to be investigated

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in the future of how we can form these

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graphite clouds

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some other points but also really

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interesting for the bulk silicate earth

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which does not have liquid water at the

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surface that's just as a reminder

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we see that we do have water clouds

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water ice clouds high up in the

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atmosphere

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and also when we just increase the

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the water abundance in that atmosphere a

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bit

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in the total element abundance but not

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allowing liquid water condensation yet

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we can drag down the water cloud base

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so that we can actually have water

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clouds at like roughly

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100 200 bar or 200 millibars

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whereas the surface is still quite still

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pretty dry

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and we actually only have water clouds

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touching the ground touching the surface

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when there is liquid water stable at the

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surface

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and that can also be seen in this plot

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when we don't have a constant surface

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pressure

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surface temperature in a way

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that we do have the exact same

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atmospheric structure for the high

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00:10:00,550 --> 00:09:59,920
atmosphere so the higher parts of the

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atmosphere

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are the same in the pressure temperature

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profile for all of these models

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but they had just have different

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atmospheric depth

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and what we see here where i just shown

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you the um show you the

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what liquid water and water ice clouds

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we see

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that basically independent of the um

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of the actual surface pressure and

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00:10:24,630 --> 00:10:22,560
surface temperature we have

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00:10:26,310 --> 00:10:24,640
the ability to have liquid water clouds

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00:10:27,190 --> 00:10:26,320
that is really interesting if one wants

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00:10:29,750 --> 00:10:27,200
to think about

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00:10:31,190 --> 00:10:29,760
some aerial biosphere some biology

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somewhere in clouds on a

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on a planet so that is already really

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interesting but the

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the second interesting part is when we

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00:10:41,190 --> 00:10:38,720
take a look at

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00:10:41,829 --> 00:10:41,200
all the other condensates that we have

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00:10:46,790 --> 00:10:41,839
in the

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00:10:47,350 --> 00:10:46,800
just want to mention the h2s cloud up

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00:10:50,470 --> 00:10:47,360
here

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00:10:52,949 --> 00:10:50,480
and that is only

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00:10:53,670 --> 00:10:52,959
appearing for the high surface uh

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00:10:55,190 --> 00:10:53,680
pressures

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00:10:56,470 --> 00:10:55,200
where we have a high surface temperature

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00:10:57,110 --> 00:10:56,480
with quite a lot of sulfur in the

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00:10:58,550 --> 00:10:57,120
atmosphere

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00:11:00,389 --> 00:10:58,560
and a lot of hydrogen in the aperture

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00:11:01,190 --> 00:11:00,399
and then we can actually form the h2s

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00:11:03,590 --> 00:11:01,200
elements

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00:11:04,550 --> 00:11:03,600
and that can be used according to these

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00:11:07,590 --> 00:11:04,560
models

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00:11:09,190 --> 00:11:07,600
um as an in potential indicator for high

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00:11:11,190 --> 00:11:09,200
surface pressures

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00:11:12,630 --> 00:11:11,200
and with that i'd like to leave you with

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my conclusions that

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only the oversaturation of

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00:11:18,069 --> 00:11:16,079
phyllosilicates can result

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00:11:20,389 --> 00:11:18,079
in stable water condensing and chemical

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00:11:21,750 --> 00:11:20,399
equilibrium at the surface

350
00:11:23,430 --> 00:11:21,760
but independent of whether or not

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00:11:25,190 --> 00:11:23,440
there's liquid water at the surface

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00:11:27,350 --> 00:11:25,200
we can have water clouds in the

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00:11:30,630 --> 00:11:27,360
atmosphere and overall

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00:11:32,550 --> 00:11:30,640
we want to use this model to

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00:11:34,150 --> 00:11:32,560
get an insight of what kind of crust

356
00:11:37,350 --> 00:11:34,160
induces what kind of clouds

357
00:11:40,310 --> 00:11:37,360
and then to basically trace back we see

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00:11:41,509 --> 00:11:40,320
cloud a and then say that could be this

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00:11:43,190 --> 00:11:41,519
kind of cloud

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00:11:45,110 --> 00:11:43,200
these kind of crosstabs thank you very

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much for listening