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[Music]

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[Applause]

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well thank you very much for this

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introduction and before diving into

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carbon dioxide reservoirs of habitable

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exoplanet water worlds let me introduce

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you what a water world is and an

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exoplanet water world will be a planet

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that has accreted a significant fraction

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of volatiles more specifically water

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without retaining a large hydrogen

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helium atmosphere so on the side you

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have examples of two interior structures

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of the suppliant water world on the left

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here okay so here you have an example of

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a water world that will be young or

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close to its star and all of the

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volatiles of vaporized in a envelope

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above the silicon and iron core and most

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of the liquid current literature

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actually focused on habitable water

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worlds where the water is condensed as

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high-pressure water ice and possibly

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this water world those habitable water

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worlds possess a global liquid water

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ocean in contact with a thinner

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atmosphere so there are several ways to

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form water worlds the habitable water

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walls could form beyond the snowline of

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their stars they could accumulate a

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comet-like amount of volatiles and then

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migrate inward and sides with the

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habitable zone of the star and

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accumulation a later accumulation of

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water by impact between planetary

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embryos is also possible and both of

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those mechanism has been played out as a

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robust production of numerical

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simulation of water wall formation a

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third mechanism would be a sub Neptune

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planets that would migrate closer to

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store close enough that it's envelope

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will be evaporating so the star would be

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an M dwarf a young and Worf and Worf

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would be a star that is cooler than the

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Sun and rather than the Sun and also

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during the young stages of M dwarf they

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are very active and this activity would

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allow just an evaporation of this

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hydrogen and helium envelope leaving

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more heavy volatiles at the at the

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surface of the planet so actually

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low-density planets in the water bowl

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size range

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has been detected in abundance by

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ground-based and space-based and mask

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diagram with all of the crosses are a

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sample of exoplanet that has been

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detected and here as a guide of the eye

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you have a line that represent a mass in

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the radius of the planet will be a

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hundred percent of ayran here you will

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be a planet that will have an iron true

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silicate an earth like iron two silicate

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ratio and here will be a planet that

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will have an earthlike core with

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equivalent amount of water on top of it

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so solar system planets are here

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represented by diamonds you have this

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earth Venus and Uranus and Neptune that

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are here and you see that there is a

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potential sample of planets here that

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could have a significant fraction of

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water in there in their interior

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structures so there has been a status

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achill analysis of this exoplanet

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population that has been performed in

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the past years however their results do

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not provide a smoking gun for Waterworld

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detection and here you have seven

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potential Waterworld targets that have

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been detected a couple of years ago

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those are a Trappist one a planetary

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system that possess potentially five

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water rich water wells that will be

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observed probably by the next surveys so

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then back to the carbon dioxide

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reservoirs don't following the mechanism

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of formation of water worlds they could

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have come at like carbon dioxide rich

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composition because usually they form

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from a material that is far from the

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from the horse star and beyond the snow

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line so this figure here is just to show

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the possible range of co2 to water ratio

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inside of the Comets and to show that

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this range is wide and most of the

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current literature focuses on relatively

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carbon dioxide for water world's so the

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question here is if we actually accretes

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a comet-like amount of co2 which which

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could be a lot we

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err this YouTube would go inside of the

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habitable Waterworld and what could be

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then the main carbon dioxide reservoir

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of those planets so what we did is that

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we developed an interior structure of

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interest ruction model for what we call

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sparkling water world co2 Plus water

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world and we try to incorporate the

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latest experimental results in our model

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so I go very fast I'm honest I won't go

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into the detail in the complicated

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pressure and temperature like phase

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diagram of water plus u2 system I just

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say that to account for all of the

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phases that could be present here we use

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a transfer point or equation of state

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that is a state-of-the-art industrial

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equation of state for water plus u2

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mixtures and one of the first

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application of our model is to estimate

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how much of co2 can be stored inside of

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the water rich layers of those water

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worlds

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so there is two possible roughly two

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possible internal structures for

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habitable water world so this is a cold

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version of a water world that has a

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shallow ocean a sick layer of clathrates

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clad raised being a crystalline

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structure of water where water from

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cages that can entrap molecules here co2

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and then a high-pressure ice and a

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harder version of a habitable water

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world would not have this clad freight

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layer and will limit our exploration

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temperature to 400k because this has

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been shown as a limit and highest

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temperature for life as we know it so

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the co2 can be dissolved in the ocean

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can be stored in clathrates

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and for this first results we consider

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the high-pressure ice is actually pure

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water ice so this is an example of

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interior structure that we get with our

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model here for the cold version I have

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the pressure and the composition of co2

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inside of the profile

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the skills here are different so for the

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colder version the shallow ocean

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actually store a few percent of co2

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while the clap the cigarette layer can

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store up to 15 percent of co2 inside of

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it for the hottest version there is a

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discrepancy between what model predicts

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and what actually all of the current

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models equation of state of water plus

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you would predict and the very recent

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experimental experimental data so here

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in Y the equation of state would protect

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a decrease in solubility of co2 in water

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for at saturation for pressures above

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100 MPA while the experimental data show

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that this solubility increases and reach

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up to 20% here at 303 GPA pressure

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so what we do is that we compute those

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profiles we sum the total amounts of co2

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that we get from those profiles and then

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we divide by the total amount of

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volatiles in the in the hydrosphere of

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the planet total amount of volatiles

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meaning water plus u2 and then we

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compare it to the possible range of

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cometary compositions here this range is

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shown in gray and this figure shows that

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first of all the hot water worlds are

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the one that store the most of co2

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inside of them so yes sir the y-axis

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here is the total planet for that

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fraction meaning that here for example

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it's a planet that accreted 50% of

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volatile by mass so I was saying that

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the hot water walls are the one that are

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able to store the highest amount of co2

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because of this increased solubility of

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co2 with depth and this red line takes

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account from it and the second a result

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that is shown in this figure is that a

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planet that has accreted more than 11

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percent of volatiles by mass are enabled

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to reach this comet-like composition

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meaning that if for example those planet

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actually accreted a comet-like

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composition of co2 so a very rich

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composition

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you chew this excess has to go somewhere

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and one of the obvious possibilities for

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this huge shoe is just go in the

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atmosphere right you have a very sleek

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atmosphere of co2 however in that case

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the water world would not be habitable

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so the radiative transfer simulation

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show that if I have more than 100 bars

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you chew inside of the inside of the

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atmosphere of a water world the

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temperature will rise above this 400k

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limit and then the habitable the water

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world would not be nice for life as we

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know it so here we propose that the

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carbon dioxide could be stored as co2

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ice or as a newly discovered carbonic

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acid monohydrate solid because both of

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the co2 ice here and this solid have

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their identities that are higher than

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the densities of high pressure ice

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meaning that they will be stable as

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stratified stable stored under those

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those layer of high pressure ice and

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away from the atmosphere and this is and

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this is what we want to preserve the

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habitability of water world so the

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question is how to get those solids

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there and we are working on it and this

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is kind of a big picture situation to

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show you one of the possible mechanism

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of what is happening to store the carbon

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dioxide inside of this water world and

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we think that actually the habitability

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of the water world might be determined

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during the cooling history of the

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planets so here you have an example of a

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water world it is of accreting that has

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a supercritical water plus u2 envelope

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uniformly mixed very hot and depending

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on the condition of the cooling of the

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water world if those conditions are

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favorable for co2 to actually rise and

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stay in the atmosphere then those water

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walls are possibly non habitable because

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we will creating those suture rich

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atmosphere with very strong greenhouse

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effects however if they can

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addition are favorable to for this you

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to sync and to form those Isis or the

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solid then this you will be trapped and

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this outcome will be possibly habitable

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okay so here's my summary so the

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atmosphere the ocean and the clathrate

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layer are actually of water worlds are

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not enough to store a comet-like amounts

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of co2 if if the water wall de created

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more than 11% of volatile by mass if you

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want to avoid a hot and on habitable

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scenario we need to sequester co2 away

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from the atmosphere inside of the

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high-pressure ice mantle and the

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habitability of a water world would

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probably depend on the cooling history

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of the planet and the extent of the

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carpenter said solids are stored inside

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of this high-pressure water ice layer

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yes thank you

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I'll be happy to up any questions for

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questions maybe come to the mic if you

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in mind because I think they're

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streaming thank you

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hi great talk thank you I was wondering

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if your model consider speciation of

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carbon dioxide as things like

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bicarbonate and carbonate that's that's

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a really good question so the model is

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pure water and co2 alright so if there

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is no other agents such as a calcium or

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like water rock interaction coming from

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Wetterich interaction this speciation

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so yeah but to lower the pH you need

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additional a to higher to put the pH

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higher you need additional agents to do

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that and the model does not account for

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them so that would be that would be

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actually great addition but I think we

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will hear about salts inside of a

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Waterworld later yeah cool see Vance JPL

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really nice work I'm glad to see you're

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using the results from a person it

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wasn't at all yeah had a question about

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the structure getting a two thousand

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kilometer thick high-pressure ice layer

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there well so there was the issue of the

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thermal profile in such a thick layer I

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would expect for a large world you've a

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lot of radiogenic heat from the interior

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and it would be hard to have a nice

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layer that thick there was isothermal

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rather than following close to the

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liquidus of the - rights

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it's just wondering what you did to

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model the temperature structure of the

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ice so yeah so the parameters of the

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model has been kind of optimized to have

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a maximum storage of co2 so what this

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slide doesn't tell is that the

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isothermal profile is only inside of the

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ocean and class right layer not inside

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of the high-pressure water ice the

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high-pressure water ice has an adiabatic

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profile actually even even in the ocean

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compressibility of the water will lead

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to a drastic temperature increase by the

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time you get to the high pressure ice

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yeah I agree but it also will lead like

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the increasing temperatures will

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decrease the solubility of Sojo so

315
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keeping those isothermal profile getting

316
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really the Apple level of the maximum of

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co2 that you can possibly either setting

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upper bound yeah exactly that's good

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so just one one quick question is the

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high pressure ice in this on the Left

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starting at ten mega Pascal or 1 mega

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Pascal I think it's starting around 600

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MPA okay okay yeah very good thanks I

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owe and lemur and I was just wondering

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00:14:42,509 --> 00:14:40,019
if your model has a sink term for

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cations coming up from the silicate

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interaction with the high-pressure ice

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or if that's something that could be put

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in so I know this model my mom does not

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account for that yet Thanks well thank

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you so much