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[Music]

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one thing I like about AB grad con is

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the audiences is pretty chill so we're

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all grad students undergrads so I get to

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experiment with how I do presentations

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so I need first I need some audience

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participation

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can someone give me a letter hey Jay

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okay another lender okay now a number

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between one mm I knew someone was gonna

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say that I'm gonna go with 13 another

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letter you okay this is great

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all right now hot or cold hot all right

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perfect

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okay so I'm going to talk about color

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I'm gonna be talking about in a couple

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of contexts all related to exoplanet

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habitability I'll be talking about how

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we can use it to classify things now and

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how I'm using it in some models to

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classify things in a future and I want

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to do it or telling the story of a

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planet just recently discovered JC 13q

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meaning it's there's many planets in

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this system it's probably the most

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impressive planetary system ever

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discovered and it has this habitable

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planet it's totally real it's there it's

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got life teeming on it but how are we

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gonna know how do we figure out that

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it's there so right now we can't really

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make detection zuv what the composition

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yeah this feels like we have a range you

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know we can detect habitability out to

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like zero lightyears

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so this planets much further than that

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so what we can do now is we sort of can

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make guesses and leader people like

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Claire will you know use telescopes to

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actually make the detection and confirm

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our guesses so as we build up these

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guesses we're sort of building a library

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of sort of pictures of what potentially

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habitable planets could look like and

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then we have this reference catalog it's

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like sort of like an Autobahn guide like

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we're building up you know reference

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pictures and then you go out in the wild

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you actually observe something and you

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try to match it as close as you can so

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the first thing you sort of want to do

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is you want to have like ground truths

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to what you wanted to do first we need

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to actually find some real planets and

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what do those look like first so we have

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a solar system that's pretty diverse we

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do have a habitable planet which is nice

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so some of the earlier work we did was

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actually look at our neighbors stuff in

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our own solar system to see what they'd

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look like as exoplanets so we calculated

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geometric adios for the 19 different

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solar system objects you you know the

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planets some dwarf planets a bunch of

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moons to sort of build this you know

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picture of what our solar system looks

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like and then we use that to model what

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they would look like around other stars

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and here's our

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JC 13 cute is down here so it doesn't

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have the spectra of x3 when I figure out

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what that's gonna be like so we reaffirm

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and rip one of the things that you can

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do with just something as simple as

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looking at our own solar system and

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that's distinguishing different types of

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surfaces it's gonna be one of the first

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steps when you find an exoplanets here's

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a rocky as a gaseous as an icy so even

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with something as simple as one of these

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colors so people might not be familiar

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with this rnj these are just different

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filter bands you essentially just take

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your spectra of the planet you have a

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filter man you just integrate over that

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and it's just this broad broad spectra

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thank you think of like a very low

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resolution spectra and this is just you

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know a reddish color and this is

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for red and here's a couple more

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infrared so even with this very low

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resolution spectral data you can

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distinguish different surface types so

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it's something we can do using objects

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in our own solar system but there's this

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can only go so far so if you have a

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planet that has any sort of atmosphere

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and you change the light source that

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chemistry is going to be a little

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different we can do things you know for

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rocky planets like that don't have much

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of an atmosphere that's not gonna change

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much in terms of its colors if you put

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on a different star you can adjust for

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how the lights going to be different

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there's no chemistry really changing the

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atmosphere because there isn't any so if

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you really want to look at something

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like our planet which is around a hot

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star so it's a lot hotter than our own

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Sun so the light that's hitting it's

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going to be different so if you look at

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the models that we're using to simulate

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what those atmospheres would look like

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for habitable exoplanets we find that

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they're they're sort of not good enough

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they do do the job of changing the

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chemistry of the atmosphere you can sort

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of model how that that light is going to

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change the chemistry but they they lack

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another key feature which is the surface

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albedo spectral information that points

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a huge role in how the climate becomes

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stable so to our model the planet kind

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of looks like this it's gray it's just

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there's no color information for the

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surface it's just a single value that

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you're using to treat the entire

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reflectivity of the surface it's a

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single number we want it to look like it

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is something like less you know much

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more close to what it's actually like

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but we do use one dimensional models so

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it's more like this and we want it to be

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like this

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so there's that still improvement and

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there's there's a good reason to believe

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that this just adding this color

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information for the surface is going to

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alter the climate over our planets a lot

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so I'll do a little bit more complicated

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albedo diagram than what amber showed so

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we have our Sun here you know all the

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incoming energy is hitting the planet

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here which is gray have our atmosphere

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and so what all these lines are telling

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you is like there's you know hitting the

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top of the atmosphere we have all the

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energy from the Sun there's some being

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absorbed by the atmosphere and reflected

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off some is being absorbed by the

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surface somes being reflected by the

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surface and here we have longer

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wavelengths the infrared being emitted

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from the warm surface absorbed by the

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atmosphere and re-emitted by the

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atmosphere or then directly you know

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radiated out into space so if we change

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the Starlight that's good we have a gray

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planet here so we don't have any

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interaction between the albedo and the

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changing star like it's gonna be pretty

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much the same we can model how the

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atmosphere is going to change here if we

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add color to the planet now we don't

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know exactly how you know there's going

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to be changes in how much is getting

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absorbed by the surface what's being

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reflected and that's it going to be

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affecting how much is then being reread

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yet but a surface and then escaping into

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space and this is where you're setting

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habitability constraints as well because

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you this is controlling you order

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surface temperature and that's gonna be

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what you need for habitability in them

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I'm saying habitability I should define

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that like surface water if you have

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water on the surface we'll call that

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habitable so to look at this in more

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we have different star spectra here so

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our planet

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JC 13q is around a hotter star so it's

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gonna be like an F star this is gonna be

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this spectra here we have microns 0.5 to

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2.5 s this is your infrared and this is

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this the relative flux for these

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different stars you have the Sun here in

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white and then a cooler start here red

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so you can see that they're emitting the

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different light is gonna be playing the

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planet around these different stories

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here down here we have the reflectance

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so this is that surface color surface

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albedo I have this dashed line is the

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flat this is what the model is used

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right now it's just a gray surface it's

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reflecting exactly the same in all

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wavelengths and here I have an earth

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model that's at the resolution of what

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our models sort of look at you do the

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radiative transfer at so let's go let's

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go for this Sun let's start with the Sun

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so if the Sun spectra is hitting the

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flat that's okay that's what our models

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had all been built to do all these

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models are coming from Earth around the

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Sun they were used to simulate the

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Earth's climate and they've been sort of

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ad hoc let's just mesh together to

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create exoplanet models um so you can

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really tell that this is something that

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is left over from you know when it was

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just being used for Earth because this

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actually simulates fairly well you know

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the surface temperature that you get

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players so that's okay if we have this

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one we can use the flat fine if we

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change the star and it's still flat

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there's really not much interaction here

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it's you can you know every every change

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that's occurring is just just captured

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by the star but if we have a changing

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albedo say this Paris model you can see

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that if we change the star we're going

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to be absorbing and reflecting different

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in different parts of the spectrum now

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that's gonna be altering our surface

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temperature so if we have a cooler star

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this M star we see that we're absorbing

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more it's albedo is lower over here

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we're more the sunlight a star lights

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hitting so we're gonna be absorbing more

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there so the planet should be hotter

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than if we had just used a flat and if

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we're around the star that our planets

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around where a lot of the flux is at

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these lower wavelengths or B we're

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reflecting a lot more so our planet

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should be cooler make sense and if we're

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using an earth model from your service o

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videos we use the Sun we should get a

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same surface temperature as we did for

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the flat because that's how the flat

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model was chosen so we expect for

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something like this albedo we expect

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cooler stars to be hotter and hotter

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stars bluer stars to be colder and

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that's exactly what we see when we

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change the models to accept this

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wavelength dependent surface that we

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don't so here I have this is temperature

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deviation from between the flat model

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and the wavelength dependent model this

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is a surface temperature deviation as

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you can see for M stars these cooler

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stars the surface temperatures are

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hotter and for the f stars the hotter

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stars the surface temperature is cooler

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this is so this is using the earth model

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comparing it to the flat so we have

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hotter cooler and the Sun the 0.3 albedo

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that you saw here that's has been around

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for a while and that's been calibrated

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to give you the same surface temperature

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as what the earth now if you had used a

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really accurate earth model so this is

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pretty big this is you know this is

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changing how you would define sort of

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if you're using wavelength dependent up

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you go

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now instead of just using a flat line if

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you had something that more represented

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what the surface actually looks like so

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what does that mean for our planet

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JC 13q it's got so many neighbors around

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and I was thinking someone is someone's

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gonna pick a really like late letter

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we're just gonna have a lot of planets

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in this system so there's probably

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multiple there's even multiple planets

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in the habitable zone for this so what

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is this mean we don't know what the

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surface is going to be for this planet

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we have an idea of what happens surface

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might look like so we could use an earth

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model but we can also look at how this

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line changes for different types of

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services maybe there's more ocean

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there's less ocean maybe there's more

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vegetation maybe there's less of

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education deserts stuff like that so we

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can sort of look at the different

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spectra that are around us use those as

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surface albedo and see how they would

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change the habitability of a planet

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using this new method internet'll so

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I'll just leave some ring up here thank

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you thank you to my discovery team for

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[Applause]

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Hey

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very cool presentation thank you are you

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planning on using your model to any

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extra work so planet any actual

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exoplanets yes

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we are using it to model some of the

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recently found exercise and what did you

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find

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well we're sort of in the parent

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luminary stages of testing it you know

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trying out different surfaces um simple

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way we've been using it for current

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exoplanets is to use something that's

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similar to earth for now but that's

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still better than using a flat so we're

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we're taking it one step at a time yeah

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okay yeah we are we are finding that you

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know it is changing so a five degree

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difference in surface temperature can be

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pretty big for habitability um so it

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does make a pretty big difference if

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you're on dem stars which are very

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hi so I know this may be kind of a silly

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question but I'm just curious if when

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you're talking about like unserviceable

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yo are you including cloud cover and yes

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we're so if we go back to this if you've

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seen a an earth albedo that's helped me

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know it's actually very low it would

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look something more like yes so this has

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clouds incorporated into its albedo to

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get it to match a surface temperature

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that is the same as what we find for so

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we use a cloud coverage of approximately

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what we see today around like 50 percent

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cloud coverage and if we do that it

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actually gives us the same surface

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temperature which was a nice check but

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it is still not it's not like a cloud

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layer in the model there is work on

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incorporating those it's a very

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difficult problem so there isn't a super

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good solution yet on how to incorporate

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it into a 1d model but it's being worked

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um on your slide where you are showing

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the different filters it looked like you

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had gas ice and rocky does that mean

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that you are not taking into account

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water world's or are they considered

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part of ice so these are just the

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planets in our own solar system there

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are objects in our own solar system ice

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there are some moons here there's a lot

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more dots than 19 because there's some

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multiple observations you know this is

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like a Neptune or something like this

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cluster so yeah each one of these is one

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of the objects in our solar system that

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I had on this but if you did have it so

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earth is pretty much it's very close to

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a water world and we put it in the rocky

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group and it it matches up which is

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interesting because water and these

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wavelength ranges looks very close to

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rock it's actually very it's just very

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dark it just absorbs everything so

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that's a lot of what these rocks

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actually look like so if that's an

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interesting question to disentangle if

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you had just these to work with how can

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you distinguish between a water world