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hello everyone

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i'm tim liechtenberg from oxford and i

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work on the formation and early

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evolution of terrestrial planets in the

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atmospheres

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my principal goal is it to better

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understand the early formation and

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evolution phase of terrestrial planets

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in order to infer something about the

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planetary environment of the haitian

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earth with the ultimate goal of better

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understand you know

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what what was the environment that

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enabled

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the origin of life on earth um but i

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think we should look out

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in order to infer something about

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ourselves

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why is that so what you see over here

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are

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scenarios of the hadi nurse

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with uh hiding earth which was a very

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defining phase

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on earth and we have no geological

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record of this

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and there's basically 500 million years

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directly after transformation that are

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completely gone and vanish

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from managed from our site um

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after the apollo mission we had this

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picture of the hedin earth very hellish

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you know frequent meteoritic

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bombardments

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uh constant volcanic outpourings but

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since

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evidence for liquid water the earth's

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surface emerged

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about very rapidly after the moon

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forming impact in fact

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the picture is you know in question and

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but still we have very little that can

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help us from a geo

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geology point of view and so what we're

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aiming to do

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is to actually look to other planetary

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systems that are still currently in that

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phase and that are young

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and that um that can inform us about how

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terrestrial planets at that stage of

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evolution evolve

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and how they look like and principal

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questions are of course for instance the

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composition of the atmosphere and the

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interior

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that can help us to inform the

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geochemistry of the surface at that

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stage

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why is that important so for instance

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here you see the interior the interior

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composition determines the amount of

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gases or the composition of the gases

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that is degassed and forms the

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atmosphere the atmosphere itself

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is also of course very important because

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it kind of sets the uv environment of

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the surface

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and it gets influenced by the radiation

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environment from the star

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and it can directly react to changes but

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for instance

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from bombardment yeah commentary or

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meteoritic bombardment

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now those two things together

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make up the geochemistry of the surface

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this directly affects the feedstocks

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that are available for prebiotic

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chemistry

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so the combining the combining link here

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is the redox state and all of them are

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set and are affected and affect

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themselves the radius redox state of the

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mantle

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and the prebiotic chemical networks that

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can play out

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on a given planet at a given stage now

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what you see on that next slide is a

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sort of confusogram but

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it shows one envision possible pathway

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of how

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terrestrial rocky planets in general

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acquire the atmospheres

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so this is time and this is the material

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and this is the atmosphere

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in the beginning i just thought that

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terrestrial rocky planets specifically

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larger ones

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still have hydrogen-rich atmospheres

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that are directly sourced from the port

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planetary disk

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the mantle is molten because from its

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secretionary heat but then solidifies

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over this over some time the primary

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atmosphere is lost due to escape

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and then it's replenished from volcanic

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outgassing that is why the composition

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of the interior is so important

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because it sets the composition of the

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gases that are released to the

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atmosphere

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now this story can be different

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depending on the composition of the

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planet and therefore

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depending on the specific accretion path

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of the planet itself

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and this changes very dramatically how

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these planets evolve

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during the earliest phase so here for

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instance you see the cooling from magma

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ocean to a habitable planet this is

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surface temperature this is cooling of

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the planet by heat loss through the

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atmosphere

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and depending on the primary composition

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of the atmosphere for instance if it's

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h2o dominated o2 dominated ch4 dominated

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to h2 dominated

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the heat loss is dramatically different

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several orders of magnitude

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this is very severe consequences for the

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surface environment

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for the geochemistry of the mantle and

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for the composition of the long left

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atmosphere

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now um that's why we develop

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computational models and actually can

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can

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quantify the differences between those

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scenarios

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this is what you see here on the right

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you see like basically the evolution of

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a magma ocean planet

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in this case an earth-sized one for an

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h2 an h2o dominated atmosphere

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so this is temperature in k depths and

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mantle height and atmosphere

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and you see the difference and cooling

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behavior of an h2 and h2o1

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from 100 year to one mega year and you

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see that

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after one mega year the surface

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temperature is strongly different very

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very starkly

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strongly differing and also this

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stratification of the atmosphere is

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different

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and these differences so strong that

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they are in the order that we can

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potentially be

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potentially resolved with astronomical

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surveys

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um not only the size is so strongly

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different but also the plant looks

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very differently this is shown on the

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left hand side uh your

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contrasting h2o again with h2 this the

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y-axis here is the spectral flux density

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for a given wavelength this is basically

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how the planet looks like

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so astronomical surveys only progress

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specific length or a specific

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area of that wavelength range and this

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here for instance

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is the wavelength range of one

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of the future direct imaging survey

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that is currently in the concept phase

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um and

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these types of service will not only be

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able

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to actually see those types of planets

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but they will also be able to infer

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something about the interior state

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these are the different lines you see

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here so i don't have the time to really

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go into the details but

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these different lines show different

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interior properties for instance how the

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magma and the solid

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rocks behave when you see their order of

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magnitude differences for differing

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crystallization path

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and order of magnitude differences

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between compositions of the atmospheres

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and so when we will be able to see those

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planets we will be able to make out

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their differences and understand

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the diversity of these early portal and

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cooling

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magma ocean atmospheres now this is

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uh for the future but at the moment the

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um the question is really what how do

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larger planets behave

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this is potentially important because

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some of them specifically this

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class of so-called supers or

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sub-neptunes is

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dominated by rock stamas and so they are

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definitely related to the terrestrial

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planets at some to some it's to some

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extent

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and uh we can actually probe them today

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and specifically with the james webb

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space telescope

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um from next year on uh this here shows

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uh

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these are two famous members of this

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class this is gj1132b for which

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there has been a claimed detection of a

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reduced atmosphere this is k218b

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for which there's evidence for water in

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its atmosphere and

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the existence of these types of

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superheroes atmospheres is very

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important specifically the long-lived

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ones after

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the portal atmosphere has escaped

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because we can then

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if they if there are reduced super

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earths we would be able to

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probe prebiotic chemistry in action

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this here for instance this model

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spectrum of this planet gj1132b

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you see that for instance with with

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jbl wst neocam instrument we would be

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able to make out

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cyanoacetylene in the atmosphere

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using different markers so this is

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something very exciting to look forward

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to

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and potentially in the next few years we

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will actually get confirmation of these

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types of observations

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now this is exciting but it's

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debated in the community the reason one

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of the reasons is

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that we actually believe these secondary

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atmospheres and super earths should not

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be reduced they should be oxidized

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why is that the reason is that larger

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planets should in principle

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tend to be more oxidized because of

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geochemical

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reactions that operate in the interior

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of these planets so the principal idea

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is that if you have like something on

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the order of a moon or mass-sized planet

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you can host a reduced atmosphere but

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the larger you go the more oxidized you

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become

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and uh one of the main reasons for that

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specifically relevant for earth-sized

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planet is iron disproportionation

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the principle reaction here goes like

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this so we react

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fe2 plus an fe2 plus phase to fe3 plus

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plus a metallic iron

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for instance while the reaction silicate

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melt plus aluminum oxide makes periscope

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plus

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metal and this metal due to gravity then

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sinks to the core

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in this net oxidized instrumental and

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this means that the gases that come

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out of the mantle are rich in water and

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water and carbon dioxide

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for instance now that is not

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that is a standard picture but it may be

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fundamentally different

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in super earth actually this is what

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i've shown earlier this year

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because um the uh

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super hours are much larger and their

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gravity is much higher the convection

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interior is actually much more vigorous

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and people have not quantified this so

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far but it turns out using scaling

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analysis

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um that that the convection is so

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vigorous

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that these metal droplets don't have to

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sink actually in the to the mantle and

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they don't merge with the core

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that means that reducing power can be

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kept in stars is in the in the in the

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mantle

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and therefore uh redu super earth can

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still

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in principle host reduced atmospheres

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with h2 ch4 and nh3

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and their photochemical derivatives and

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this predicts that actually if

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magma oceans the magma dynamics and

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super earth should work like this

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then we would expect to see reduced

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surfaces versus in this case we would

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expect oxidized surfaces and because

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this this scenario enhances the chances

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for detection on long-lived reduced

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atmospheres

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we should in principle be able to probe

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this with near future observations

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now the uh prospect for observing

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surfaces actually very exciting

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and it probably has been done already uh

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for the specific famous case of lhs

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3844b

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he used the temperature map of the

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planetary surface from a very long

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spitzer space telescope

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campaign and this was the first planet

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for which we have actually temperature

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boundary conditions now from this

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temperature map here

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so here's the star this planet is

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tightly locked surface it's now facing

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site is in an eternal day it's hot but

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not molten

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and the night side is eternal night and

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it's freezing cold there's no atmosphere

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around so it's basically direct space

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boundary conditions

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because this was the first time we

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actually have a boundary condition for

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um for a super earth we use that and try

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to infer the geodynamic mode of that

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planet

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it turns out it's fundamentally

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different from anything that we see in

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the solar system

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this is what you see over here so here's

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the star this is a cut through the

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planet

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and this is a geodynamic model so what

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you see is basically the flow of the

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rock

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inside this is a solid state convection

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here's the metal core

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and here's the surface of the planet you

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see upwellings in the dayside

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and cold down wellings on the night side

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this is actually not a preferred model

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because we think that the

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lithosphere on these types of plants

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should be very strong in that case

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something

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very unintuitive happens namely that

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actually the day side is the prominent

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location for downwellings

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and the the night side actually should

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feature

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more upwellings and therefore also

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volcanic outpourings

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and this actually predicts that the

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volatile recycling pattern

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on these types of planets should go like

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depicted here so from the day side

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down to the mantle and through volcanic

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outgassing be released again on the

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night side

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and this is again something that we will

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be able to observe with jwst

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specifically this planet is targeted for

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a observation campaign next year

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and with that um i want to finish um

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and just to summarize so hopefully we

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will be able

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uh using astronomical observations to

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infer the composition of secondary

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atmosphere

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which constrains the mental redox state

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and volatile budget

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and tells us something about the

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interaction with hot molten mantles and

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the atmospheres

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and therefore informs the planetary

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environment of the aden earth