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my name is Bailey word well I work for

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ben Brown and Jeff oishi here on campus

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and what I'm going to be talking to you

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about today is dynamics in chemistry of

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X planet and here's to dehydration

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simulations that's the talk title I came

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up with several months ago I decided I

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should probably give you a talk title

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that is actually informative about what

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I'm trying to convey in this talk and

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what I want you to learn about in this

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talk is why you should care about jovian

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planets or gas giants when you're

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interested in astrobiology so to start

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off with the major focus for people who

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are studying exoplanets right now is the

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F coming telescope jwst or the james

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webb space telescope and the reason why

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we're so excited about this telescope is

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this telescope is a next-generation

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infrared telescope which means that it's

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going to be focusing on the light that

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exoplanets are brightest in so when

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you're observing an exoplanet and you

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want to observe its atmospheric spectro

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so you want to get an idea of its

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composition what you're looking at is

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you're looking at the small variations

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induced in the transit due to the light

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due to the plant absorbing excess of the

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star's light or absorbing less of the

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star's light and so those excesses

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change the typical transit depths where

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you're looking at a typical transit for

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a jovian planets on the order of one

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percent for an earth-like planets on the

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order of about a hundred percent or

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forty hundredth of a percent for if it's

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around an m-dwarf if you're looking at

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Mysterio differences those are on the

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order for those percents of those

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percents and so it suddenly becomes much

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much harder to get details about an

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earth-like planet than a Jovian planet

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the other thing is that on JWC we're

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limited for time because the entire

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astronomy community is using jwst and so

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if you break down the timescale of its

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primary mission we have about 300 days

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to observe exoplanets what that means is

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that we can characterize the atmospheric

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structure for 150 jovian planets or

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three years like planets and so

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especially because we're only going to

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discover these arts like targets two

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years in TJ WCS mission we're going to

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be observing a lot of jovian planets and

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I want you to realize that that's

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actually going to be a good thing for us

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so let me take an aside for one second

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and explain the minimum a solar nebula

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model so the minimum mass so a nebula

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model is our Bay

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a starting point for the evolution of

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the solar system from where it was

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forming what we do is we take the mass

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and the composition of every planet we

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smear it out along its orbit and we had

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basically interpolate between those

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points and say this is what the third

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planetary disc of the solar system look

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like but when we're looking at so

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planets we're looking at a whole range

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of kinds of stars with different levels

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of heavy heavy element composition or

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metallicities and so we don't have a

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good idea of how they're protoplanetary

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disks should look except for something

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through things like Alma observations

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what we can use to jump in between that

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is jovian planets when we look at the

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composition of jovian planets we get

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data points across the disk for what the

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composition is and this can allow us to

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make inferences for what the composition

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of earth-like planets should be based on

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the relationship between the jovian

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planets metallicity and the metallicity

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of these stars so when we're looking at

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jovian planets composition we

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specifically focus on something called

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the carbon oxygen ratio and there's two

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ways of deriving this ratio one way is

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to take the observer's route and to

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observe all the carbon bearing molecules

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and all the oxygen very molecules some

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of them up take the ratio the other way

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to do this is to take the theorists

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route and do Ford modeling so you model

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the elemental abundances see how that

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carries through to the molecular

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abundances and compare the spectra and

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do a fit the problem with this is that

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when you're doing the theoretical model

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you actually have to assume some way the

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elemental abundances tie to molecular

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abundances and you can say that

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everything is nice and in thermal

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chemical equilibrium or you can say that

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it's complex and the dynamics affect how

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much of everything you're going to see

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and assume that kind of model so when

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we're trying to assume that the dynamics

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affects things because we know from

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Jupiter that the dynamics do affect the

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concentrations of molecules that you're

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seeing we use an approximation called

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the quenching approximation and what the

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quenching approximation does is it uses

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in analytical theory called mixing like

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theory which describes how the

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atmosphere boils essentially it

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describes how it convex and for the

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typical reaction we consider which is

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the carbon monoxide methane in a row

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conversion reaction when we do is we say

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there's a certain time scale that

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describes the motion of the atmosphere

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at a certain time scale that describes

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the

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reactions and when those time scales are

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equal the motions of the atmosphere are

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going to interfere with the ability of

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these molecules to react we can then do

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a lot of maths and partial differential

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equations arrived with a profile how

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everything is going to go up in the

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atmosphere if you want to do that math

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later that's fine taking it by word and

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we can make the assumption that the time

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scale or these are the scale at which

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the time scale will chemical reaction is

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slowing down as you go up in the

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atmosphere is very very small compared

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to the wit rate at which the dynamics of

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the atmosphere are changing and when you

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do that everything right here on the

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right-hand side drops off and becomes

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one and you just get that the

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composition above the clench point where

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the time scales are equal is constant

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and so that creates differences like you

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see here where you have a nice squirrel

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to the carbon dioxide for this one and a

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nice straight line right here and so

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that vary significantly impacts what

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kind of abundance is we infer for these

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planets because it's an order of

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magnitude difference in the

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concentration but there's something else

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we have to consider and that's the

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Jovian atmospheres aren't just a fully

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convecting they have a conductive zone

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at the bottom and that convective zone

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drives dynamics in an upper radiative

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zone it arrived something called gravity

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waves which have a very different mixing

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behavior than the convection and when we

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try to apply something like the punch

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approximation to the radiative zone

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there is no theoretical basis for it to

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apply now that's okay if our

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observations that have the light coming

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from the convection zone but simulations

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of jay davis t show that they don't they

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actually we're if red is where all the

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light is coming from they are coming

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from very high up in the radiative zone

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which means that we have to consider the

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mixing due to the gravitational waves

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and that's what I'm focusing on so I'm

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looking at how we can apply our

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understanding of gravity waves to

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chemical disequilibrium and therefore

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getting better abundances for these

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planets the way I do this is I use a

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code called Daedalus now Daedalus isn't

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something like a fully developed GCM

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code that super that is focused on one

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thing it's a you can see if my very

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wordy sent

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here a fully paralyzed pseudo spectral

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differential equation solver implement

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in Python with intuitive and flexible

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equation implementation that is my grant

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proposal sentence I'm sorry for lifting

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it upon you basically what it means is

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that this code can solve any set of

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partial differential equations and

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integrate them in time efficiently and

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what that means is when we're trying to

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work on it with an atmosphere we want to

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solve the fluids equations we can do

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this in a way that is both simple to

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implement very flexible and is intuitive

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for a user because you can take an

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equation like this and implement it like

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this where it's very easy to see which

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terms match to which terms and so that's

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useful because we can add things like

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this equation where we have tracers that

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in that simulate chemical reactants so

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what my experiment is is I'm taking

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polynomials and mimicking a temperature

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pressure profile like that of Jupiter

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I'm mimicking chemical abundance

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profiles like that we derive for Jupiter

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with a tan function and then I'm adding

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some tracers so I'm adding a tracer that

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doesn't react at all so it's just

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following the fluid motions showing how

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we thanks mix and I'm adding a tracer

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that has some reaction term so it's

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produced and it's lost and I'm sorry to

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all what chemists in the room what I'm

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doing is I'm saying that most reactions

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are fast compared to a single reaction

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and that does work for the quench

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approximation and I could show you the

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mathematical proof to say that that's

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okay but it makes them something there's

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something that is easy to grapple for an

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astronomer so what I do is I say that I

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have an abstract chemical reaction

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defined by a chemical reynolds number

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and that's just the ratio of the

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diffusion time to the chemical time

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scale and I say if the chemical time

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scale is on the same time scale as the

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dynamics what happens this is where we

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get to my very preliminary results these

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are starting this whole thing off pretty

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recently so what you can see here is

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this is the same setup as I had in my

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slide talking about Daedalus so at the

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bottom there is a conductive zone at the

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top there is a radiative zone

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this graph right here is showing a

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mixing a measure so it's showing

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enstrophy for those of you to do physics

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that's vorticity squared but basically

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what showing is how strongly things are

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mixing up here i have my passive tracer

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and down here i have my tracer that has

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some sort of reaction going on and i

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know this color scheme is terrible i was

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trying to pick out very small scale

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motions for the reactive tracer but

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what's interesting that you're seeing is

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okay here those little fluctuations are

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gravity waves up here you can see that

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we started off with a lot of stuff in

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the bottom and nothing at the top and

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nothing for the passive tracer gets

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through to the top so it doesn't get

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carried into the radiative zone at all

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for the reacting tracer the top of the

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radiative zone does get penetrated a

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little bit but we don't have some point

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in the bottom getting held constant all

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the way through and this means that the

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punch approximation as far as we can

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tell so far doesn't work for a radiative

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zone this is very preliminary because as

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you can tell some of these

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concentrations become negative for the

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reacting scalar that is something that I

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know how to fix but has not been run yet

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because the my super computer is not

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obeying me right now but I think both of

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these both of the passive tracer and

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reactive tracer have implement

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interesting implications for emission

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like jwst and we have a lot of work to

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do before it gets up in the air we start

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observing these driving atmospheres

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questions hi can you hear me yep um I

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was wondering why you want to use Jovian

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atmospheres to trace the disk structure

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rather than something like Alma so you

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can you definitely can use all that but

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almost talking when you're looking at

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with Alma you're looking at disks that

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are typically fairly young whereas

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driven atmospheres give you a point in

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time farther in the history of the

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evolution of these disks it also gives

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you a lot of data points because you can

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observe a lot of jovian planets so it's

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kind of a complementary method to being

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able to do nice observations with

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something like Alma that can really

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reserved resolve molecules Thanks so

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does your model account for forming

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things like Hayes's that definitely mess

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with the retrieved abundances and

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probably some of the reactivity so I'm

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interested in moving on to Hazel's and

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clouds in further along on my PhD

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partially because to do that I have to

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think about nucleation processes and

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phase transitions and at the moment I

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want to understand a simpler case where

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I just have it reacting a tracer that's

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interconverting with eight with

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does your reactive tracer is it

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exothermic or endothermic as far as the

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reaction properties so because we're not

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considering really so what we don't have

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any terms for energy released by the

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reaction because it's assume that the

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energy release is very small that's

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another thing that I'm planning on

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adding and in the future currently the

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there is no back reaction of D tracer on

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the dynamics at all it doesn't affect

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the major fluid so it doesn't affect the

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molecular hydrogen and it doesn't

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release any energy releasing energy is

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the next step after we understand some

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of the implications of how reacting at

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all changes where the tracer is located

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okay so it's just in your inner

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converting between species okay any

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I'm missing something but what exactly

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do you mean by gravity waves okay so

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gravity waves are basically

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perturbations in the density that get

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carried by the gravity got it not actual

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spatial we got time for one more unless

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he just asked your question how do you

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set up the initial concentrations and

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the other boundary conditions so

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currently the initial concentrations are

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something that imply and what's right

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now I'm putting everything in the

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convection zone and just seeing if I can

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get anything up to the radiative zone

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and as part of the reason we're reaching

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negative concentrations right now is

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that the initial conditions I don't

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think work very well with my reaction

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law and I need to adjust how I'm doing

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the reaction to have an extra loss term

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for the equilibrium profile but in the

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future I'm going to also flip that over

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and see if anything get from the

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radiative zone and over and in terms of

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boundary conditions rather than

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constraining the concentrations of our

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reactant we're actually constraining its

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gradient so we're saying that there's no

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diffusion of that molecule across the

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boundary the right hands the right and

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left hand side boundary conditions

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rather than the top and bottom are