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[Music]

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hello everyone

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first I would like to start by thanking

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the organizers for the opportunity to

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give this talk so as we said today I

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will be talking about what we can learn

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about atmospheric dynamics especially in

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the upper exoplanet atmospheres and as a

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result as a result of that of what we

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can learn about atmospheric escape by

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looking at transit observing transits of

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exoplanets in one particular line of

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helium around 1 micron so j/o a little

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bit messed up ok James gave a beautiful

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overview of this entire topic and he

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saved me a lot of work so basically I

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can skip my entire introduction so he

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introduced hydrodynamic escaping close

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and exoplanets all just quickly

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reiterate these highly radiated planets

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planets absorbed a lot of high-energy

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radiation their atmospheres get heated

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up and as a result they have this radial

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outflows that can be very efficient at

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removing gas from planets and this can

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have important consequences for the

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demographics of exoplanets that we

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observe for this sub Jupiter desert and

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this radius Valley so one way to create

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these features is to atmospheric escape

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but also as James pointed out there are

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a lot of things we don't understand yet

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about atmospheric escape and a lot of

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that is because we can have not observed

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it in action until now in large samples

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of exoplanet

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so things like how does exactly mass

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flow rate depend on various properties

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of the planet and its host star so mass

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radius incident walks at different

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wavelengths age spectral type so on what

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is that heating efficiency

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maybe we can empirically derive it and

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see how it compared star through

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theoretical expectations then how

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important there are other non-thermal

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mechanisms of atmospheric escapes and

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then of course the what role do magnetic

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fields or stellar winds play in this

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entire picture so basically I think that

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one

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really good way to start answering all

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these questions is by observing

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atmospheric escape in action as it

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happens and to do that the best place to

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look are these uppermost layers of

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planetary atmosphere so we're talking

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about really really far out somewhere

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around few planetary radii regions so

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basically around the Roche radius of the

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planet or even maybe beyond and these

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are really really low density

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environments so in order to observe

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these regions in transit you have to

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look at very specific wavelength so

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perform transition spectroscopy at

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wavelengths such as lyman-alpha as also

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James mentioned and show this figure

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already so this has been done basically

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in the last 15 years since this papers

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in 2003 2004 lyman-alpha transits have

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been observed in exactly four planets in

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these 15 years and this just tells you

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how difficult these measurements are

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because stars are most like the planet

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hosting stars are intrinsically bright

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intrinsically very faint at these

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wavelengths and we lose a lot of also

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information in the central part of the

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lyman-alpha due to the I am absorption

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so we've seen this picture before from

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Ehrenreich at all 2015 it's the

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lyman-alpha flux of GJ 436b black is out

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of transit and in red is in transit and

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even just by eye we see this enormous

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drop in flux due to this highly extended

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cloud of hydrogen that's surrounding GJ

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436b so these observations have been

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great because they were first evidence

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of the fact that this hydrogen envelopes

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can extend very very far out from the

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planet where this gas is clearly no

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longer bound to the planet so this is

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direct evidence of atmospheric escape

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but as I mentioned there's a lot of

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observational challenges with observing

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lyman-alpha and some of it is that we

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actually cannot observe the center of

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the line where

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lot of really interesting information is

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contained because basically in

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lyman-alpha we mostly see just this high

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velocity high velocity tail of the

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distribution so we see particles very

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far out from the planet that have been

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accelerated to the large velocities but

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we don't really see what goes on closer

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to the planet where these winds and now

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flows are actually generated and where a

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lot of interesting physics goes on that

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we would like to understand better so

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this is my main challenge with

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lyman-alpha and so we could start

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thinking so okay what are the other lore

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some other lines that we could use to

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make these observations and learn more

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about opera exoplanet atmospheres and

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Atmospheric escape so there are a few

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requirements that we would like our line

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to satisfy so first of all one necessary

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criterion is it needs to be sensitive to

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low density gap because we really want

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to know what goes on very far out from

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the planet but at the same time we don't

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want a line that's also very sensitive

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to ISO absorption so we want something

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that is very sensitive to low density

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gas but not so much that it gets

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basically eaten away by is M on its way

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towards us and another requirement it

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would be really nice if it was

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observable from the ground

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unlike lyman-alpha which can only be

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observed with the Hubble Space Telescope

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basically now because then we have many

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more telescopes available to us and we

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can observe much larger samples of

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planets and learn a lot more and it

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turns out there is at least one line and

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hopefully more of them that satisfies

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all of these conditions and that is the

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helium line at 1083 nanometers so

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actually the origin of this line is

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really really interesting from just the

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atomic physics point of view so it comes

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to the fact that helium atoms can exist

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in two configurations based on the

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relative orientation of spin of its two

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electrons so if the spins are

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anti-parallel we're talking about the

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single end configuration if they're

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parallel we have a triplet configuration

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and these two configurations basically

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live in the

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and looking of each other because

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they're not radiatively they're

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radiatively be coupled they're still

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collisional II am Adams in transition

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between a singlet and triplet but

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radiative transitions are expressed

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which means that the lowest lying state

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of the triplet helium which is shown

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here is which is very oddly decoupled

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from the ground state has an extremely

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long lifetime and is metastable and if

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you basically look think of triplet

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helium you can almost think of it as a

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separate species and this would be it's

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in a ground state so so-called ground

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state of triple of helium and because

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it's so high up it's basically 20

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electron volts higher than the ground

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state all these transitions happen in

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either visible or near-infrared which is

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really convenient for serving them from

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the ground whereas transitions from the

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actual ground state of helium are all

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the way in the extreme UV and the

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basically the strongest transition

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originating from this metastable state

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is this one and it has the wavelength of

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1080 3 nanometers and this line has been

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well known and studied in astronomy in

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in studies of the Sun of stars and

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stellar winds in the studies of Aegean

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outflows and it has even been suggested

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as a good program exoplanet atmospheres

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in 2000 by figure in Sackville but until

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recently that has not been a lot of work

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done on it so when I started working on

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this topic basically the only paper that

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I could find in the literature that

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discusses actually the talks about an

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attempt to observe this line was this

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paper from 2003 that reported a non

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detection and after that almost as if

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the line has been forgotten until

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recently so basically what I was

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interested in is trying to see how much

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absorption in this line can we expect

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from these uppermost layers of exoplanet

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atmosphere so the thermosphere and

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exosphere and it's important to keep in

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mind that the conditions in these parts

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are very

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very different than conditions in lower

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regions of atmosphere which most people

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think about when they talk about

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exoplanet atmosphere so in thermo

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spheres we talk about really low

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densities and temperatures of 100,000

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even 10,000 degrees and this because of

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its so low density the population of

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atomic levels it's not in local

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hydrodynamic equilibrium

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so you basically need to do a non LCE

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radiative transfer to actually compute

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the population level of that metastable

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helium so basically I decided to do that

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and first I assumed a simple atmospheric

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model based on isothermal Parker wind

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which is a model that was developed back

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in the 50s to describe solar wind but

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now we believe it's actually really good

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approximation for these planetary

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outflows so basically the density

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profile looks like this it starts off a

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fairly similar to a hydrostatic

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atmosphere and evenning drops off faster

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and the Velata static atmosphere has a

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radial velocity which starts off at very

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small values close to the planet and

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then at sonic point transitions and

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become super sonic and so in in that

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kind of environment

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alcohol calc I calculated the expected

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population level of the metastable

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triple helium and found that we can

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expect to see these kinds of absorption

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signals so even though I keep calling it

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the helium line it's actually a triplet

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of line which gives us this very

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characteristic shape so it has three

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lines of these are the wavelengths so

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two components are very very close

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together and they blend in this red

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component or main component and the

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third line is further out into the blue

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so it has this carrot very

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characteristic double double peak

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profile so basically as I was finishing

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this purely theoretical work completely

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independently Jessica's fake who was

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who's here actually and she was at that

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time a PhD student at the University of

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Exeter was looking at

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Space Telescope data of what 1:07 be and

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she noted that there's this really

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strong speak and transit depth around 1

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micron and she realized that this could

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be due to the this helium line

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unfortunately due to the resolution of

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Hubble Space Telescope we've see three

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the line is not resolved so basically

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this entire band says is something like

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hundred angstrom whereas if you look at

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this line profile the line is maybe one

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or two angstrom wide so basically in

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this in Hubble Hubble data we cannot

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resolve the line but we can still detect

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that there's something strongly

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absorbing in this entire band path and I

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would just like to quickly mention that

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Megan Mansfield also observe helium

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excess helium absorption in had P 11 in

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another Hubble data set so because in

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the house in a couple data the line is

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unresolved we cannot really tell much

279
00:12:14,180 --> 00:12:12,029
beyond just the equivalent width of the

280
00:12:17,150 --> 00:12:14,190
line and we can't say something about

281
00:12:19,480 --> 00:12:17,160
how this gas is just distributed so this

282
00:12:22,310 --> 00:12:19,490
is another plot from Jessica's paper

283
00:12:25,460 --> 00:12:22,320
that shows how we use two different

284
00:12:27,949 --> 00:12:25,470
models to try to model the signal so one

285
00:12:30,470 --> 00:12:27,959
is the model that I described Parker

286
00:12:32,449 --> 00:12:30,480
when that's fairly spherically symmetric

287
00:12:36,470 --> 00:12:32,459
and it produces this double shaped

288
00:12:39,829 --> 00:12:36,480
profile and another model is by Vincent

289
00:12:42,170 --> 00:12:39,839
Berea that is quite different in

290
00:12:46,850 --> 00:12:42,180
geometry so it has this elongated tail

291
00:12:49,100 --> 00:12:46,860
of material and producers entail in the

292
00:12:51,019 --> 00:12:49,110
absorption feature and with the Hubble

293
00:12:55,310 --> 00:12:51,029
data alone we cannot distinguish between

294
00:12:57,230 --> 00:12:55,320
do these two geometries but luckily the

295
00:13:00,199 --> 00:12:57,240
helium line can be observed from the

296
00:13:02,030 --> 00:13:00,209
ground with many high-resolution

297
00:13:04,220 --> 00:13:02,040
spectrograph and this is not a complete

298
00:13:06,470 --> 00:13:04,230
list and I apologize if I did not

299
00:13:07,759 --> 00:13:06,480
include your favorite spectrograph but

300
00:13:09,920 --> 00:13:07,769
this is just to show that there are many

301
00:13:14,269 --> 00:13:09,930
out there and we can use basically all

302
00:13:16,460 --> 00:13:14,279
of them to look at transit and this have

303
00:13:18,530 --> 00:13:16,470
been done since last year for so and

304
00:13:21,230 --> 00:13:18,540
helium one has been detected a high

305
00:13:22,370 --> 00:13:21,240
spectral resolution in several planets

306
00:13:23,990 --> 00:13:22,380
and this is a

307
00:13:28,100 --> 00:13:24,000
beautiful work done all with the

308
00:13:30,680 --> 00:13:28,110
terminus spectrograph in Spain and so I

309
00:13:33,260 --> 00:13:30,690
would just quickly like to go through a

310
00:13:37,940 --> 00:13:33,270
few really interesting examples so this

311
00:13:40,160 --> 00:13:37,950
is what's 69b and this is worked by Lisa

312
00:13:42,620 --> 00:13:40,170
Northman and please see her posters I

313
00:13:45,740 --> 00:13:42,630
think today so this is a really

314
00:13:48,320 --> 00:13:45,750
interesting an interesting case because

315
00:13:50,540 --> 00:13:48,330
it has it produces about three and a

316
00:13:52,640 --> 00:13:50,550
half almost four percent transient up

317
00:13:57,320 --> 00:13:52,650
transit depth at the center of the

318
00:14:00,890 --> 00:13:57,330
helium line the line I forgot to mention

319
00:14:02,900 --> 00:14:00,900
a big the line ratio between the main

320
00:14:04,520 --> 00:14:02,910
components and the weeks component you

321
00:14:06,620 --> 00:14:04,530
can tell us a lot about the optical

322
00:14:08,870 --> 00:14:06,630
depth of the medium and in this line

323
00:14:11,180 --> 00:14:08,880
it's interesting because it points to an

324
00:14:13,700 --> 00:14:11,190
optically thin atmosphere which we will

325
00:14:16,730 --> 00:14:13,710
see later is not always the case but it

326
00:14:19,220 --> 00:14:16,740
was 69 it is and it's the only one of

327
00:14:22,670 --> 00:14:19,230
the planets observed so far that shows

328
00:14:25,100 --> 00:14:22,680
evidence of a delayed egress compared to

329
00:14:27,470 --> 00:14:25,110
address of the in most other cases the

330
00:14:30,860 --> 00:14:27,480
light curve looks fairly symmetric but

331
00:14:33,380 --> 00:14:30,870
what 69 seems to have a tail of helium

332
00:14:36,200 --> 00:14:33,390
that it takes about 20 minutes longer to

333
00:14:38,030 --> 00:14:36,210
egress than it is when it's in ingress

334
00:14:41,390 --> 00:14:38,040
so it's quite unusual in that sense

335
00:14:45,350 --> 00:14:41,400
that's really interesting another

336
00:14:49,940 --> 00:14:45,360
interesting example at HD 189 73 B we

337
00:14:53,630 --> 00:14:49,950
well-known hot Jupiter it has a smaller

338
00:14:57,500 --> 00:14:53,640
chance of depth of maybe goes up to

339
00:15:00,550 --> 00:14:57,510
about 1% in the align center but this

340
00:15:03,080 --> 00:15:00,560
planet has a really unusual line ratio

341
00:15:04,700 --> 00:15:03,090
the light in the ratio between the main

342
00:15:08,780 --> 00:15:04,710
component and the weak component is

343
00:15:11,060 --> 00:15:08,790
something I think three to one or which

344
00:15:13,960 --> 00:15:11,070
points to a medium of optical depth

345
00:15:18,380 --> 00:15:13,970
around three so it's actually really

346
00:15:20,390 --> 00:15:18,390
dense the signal goes through a dense

347
00:15:23,120 --> 00:15:20,400
medium and optical effect medium which

348
00:15:26,450 --> 00:15:23,130
is quite interesting and different from

349
00:15:28,910 --> 00:15:26,460
what 69b for example and so I hope you

350
00:15:32,170 --> 00:15:28,920
all got a chance on Monday to see you

351
00:15:35,420 --> 00:15:32,180
posters by Gloria and Antoine who

352
00:15:36,140 --> 00:15:35,430
presented the sections of helium in this

353
00:15:38,540 --> 00:15:36,150
planet we

354
00:15:40,940 --> 00:15:38,550
to two different spectrographs on two

355
00:15:43,550 --> 00:15:40,950
different telescopes so this is uh this

356
00:15:48,260 --> 00:15:43,560
is not really being done with multiple

357
00:15:51,050 --> 00:15:48,270
telescopes around the world and to go

358
00:15:53,990 --> 00:15:51,060
back to what 107 B which was that first

359
00:15:56,030 --> 00:15:54,000
detection by Jessica it has been

360
00:15:59,090 --> 00:15:56,040
observed from the ground by a large at

361
00:16:02,990 --> 00:15:59,100
all published just earlier this year and

362
00:16:05,060 --> 00:16:03,000
it still shows the high the highest

363
00:16:07,460 --> 00:16:05,070
chance of depth depth of all the planets

364
00:16:09,350 --> 00:16:07,470
so basically it reaches up to almost

365
00:16:13,480 --> 00:16:09,360
like seven or eight percent in the line

366
00:16:17,510 --> 00:16:13,490
Center so which is quite extraordinary

367
00:16:20,240 --> 00:16:17,520
so we observed also the same planet with

368
00:16:22,100 --> 00:16:20,250
kick with the NIRSPEC spectrograph on

369
00:16:24,800 --> 00:16:22,110
the Keck telescope so this is work done

370
00:16:26,930 --> 00:16:24,810
with Jessica and Lynn Hillenbrand from

371
00:16:28,880 --> 00:16:26,940
Caltech and this is still work in

372
00:16:31,430 --> 00:16:28,890
progress but I just wanted to show our

373
00:16:34,760 --> 00:16:31,440
what I think beautiful spectra is so

374
00:16:38,570 --> 00:16:34,770
here in black you see out of transit

375
00:16:41,120 --> 00:16:38,580
spectrum of was one of seven and then in

376
00:16:45,530 --> 00:16:41,130
red is the in transit spectrum which

377
00:16:49,580 --> 00:16:45,540
even by I just see this increase in

378
00:16:52,520 --> 00:16:49,590
absorption so when we look at just the

379
00:16:55,550 --> 00:16:52,530
average in transit spectrum this is what

380
00:16:57,320 --> 00:16:55,560
we get so we have slightly at lower

381
00:17:00,740 --> 00:16:57,330
version spectral resolution than the car

382
00:17:02,450 --> 00:17:00,750
Menace so we don't our line is not as

383
00:17:05,920 --> 00:17:02,460
deep because it's kind of smeared out

384
00:17:08,360 --> 00:17:05,930
but we get something like five percent

385
00:17:12,260 --> 00:17:08,370
trying to death at the line Center which

386
00:17:15,079 --> 00:17:12,270
if we assume is due to just an opaque

387
00:17:17,510 --> 00:17:15,089
like annulus it will correspond to

388
00:17:20,050 --> 00:17:17,520
equivalent radius of about to planetary

389
00:17:24,290 --> 00:17:20,060
radii so that's how far out we see

390
00:17:27,110 --> 00:17:24,300
helium at least and the transit depths

391
00:17:29,420 --> 00:17:27,120
are consistent with speak at all Hubble

392
00:17:32,420 --> 00:17:29,430
detection and allure to the owl Jimenez

393
00:17:34,970 --> 00:17:32,430
detection which were and this so they

394
00:17:37,310 --> 00:17:34,980
were taken within like a year and a half

395
00:17:40,250 --> 00:17:37,320
apart which corresponds to something

396
00:17:42,470 --> 00:17:40,260
like hundred orbital periods and the

397
00:17:45,020 --> 00:17:42,480
stealth of this signal is repeatable and

398
00:17:47,870 --> 00:17:45,030
stable for at least that many orbital

399
00:17:50,390 --> 00:17:47,880
periods and again we see a quite

400
00:17:53,049 --> 00:17:50,400
interesting line ratio of

401
00:17:56,840 --> 00:17:53,059
so the main component is four times

402
00:17:58,190 --> 00:17:56,850
stronger than the weak component and I

403
00:18:00,580 --> 00:17:58,200
will remind you in the optically thin

404
00:18:03,710 --> 00:18:00,590
median would expect it to be eight times

405
00:18:07,280 --> 00:18:03,720
deeper and so this tells us that it was

406
00:18:14,720 --> 00:18:07,290
107 we this corresponds to optical depth

407
00:18:15,919 --> 00:18:14,730
or about 2 so and then if we I think

408
00:18:17,720 --> 00:18:15,929
this is the probably the most

409
00:18:20,390 --> 00:18:17,730
interesting part of these observation is

410
00:18:23,539 --> 00:18:20,400
instead of just looking at the average

411
00:18:27,080 --> 00:18:23,549
in transit absorption spectrum if we try

412
00:18:30,250 --> 00:18:27,090
to break out spectra into time series

413
00:18:32,720 --> 00:18:30,260
and kind of group together all our

414
00:18:36,409 --> 00:18:32,730
spectra that were at the in the first

415
00:18:38,690 --> 00:18:36,419
maybe quarter of the transits then this

416
00:18:40,970 --> 00:18:38,700
shows the central partial part of the

417
00:18:42,770 --> 00:18:40,980
trends in central middle and this is the

418
00:18:46,610 --> 00:18:42,780
last part of the chance of including

419
00:18:50,810 --> 00:18:46,620
egress we see quite significant shifts

420
00:18:52,640 --> 00:18:50,820
in the line so the line starts first

421
00:18:55,100 --> 00:18:52,650
it's red shifted corresponding with

422
00:18:57,260 --> 00:18:55,110
respect to the rest frame wavelength

423
00:19:00,110 --> 00:18:57,270
then during the mid transits it's kind

424
00:19:02,690 --> 00:19:00,120
of right in the rest frame and then in

425
00:19:05,900 --> 00:19:02,700
in the later part of the transit the

426
00:19:09,530 --> 00:19:05,910
line is blue shifted and this has

427
00:19:13,539 --> 00:19:09,540
actually been seen before and or similar

428
00:19:19,280 --> 00:19:13,549
pressing the floor in was 69 and HD 189

429
00:19:20,539 --> 00:19:19,290
with almost similar shifts and this is

430
00:19:23,180 --> 00:19:20,549
telling us something really interesting

431
00:19:25,340 --> 00:19:23,190
about the dynamics of these upper layers

432
00:19:28,220 --> 00:19:25,350
of planetary atmospheres and it's also

433
00:19:31,190 --> 00:19:28,230
telling us that our simple model based

434
00:19:33,680 --> 00:19:31,200
on very symmetric part or winds are just

435
00:19:36,140 --> 00:19:33,690
not enough are not sufficient to explain

436
00:19:39,440 --> 00:19:36,150
these data so basically here I just

437
00:19:42,650 --> 00:19:39,450
demonstrate how if I take this my very

438
00:19:45,200 --> 00:19:42,660
symmetric part Irwin that just has a an

439
00:19:47,690 --> 00:19:45,210
outflow but it's all just the same in

440
00:19:50,000 --> 00:19:47,700
all directions and it kind of you can

441
00:19:51,890 --> 00:19:50,010
reproduce you can find a model that fits

442
00:19:53,930 --> 00:19:51,900
the mid trend so it's kind of fairly

443
00:19:56,690 --> 00:19:53,940
well but if you try to use the same

444
00:20:00,590 --> 00:19:56,700
model to reproduce the earlier phases

445
00:20:02,930 --> 00:20:00,600
the kind of ingress and egress you fail

446
00:20:03,870 --> 00:20:02,940
so it's basically telling us that we

447
00:20:05,789 --> 00:20:03,880
need to make our

448
00:20:08,760 --> 00:20:05,799
more complicated and add additional

449
00:20:10,560 --> 00:20:08,770
physics and learn the data is already

450
00:20:12,240 --> 00:20:10,570
rich enough to tell us more about the

451
00:20:14,640 --> 00:20:12,250
system than just what the simplest

452
00:20:19,169 --> 00:20:14,650
models are capable to tell us which is

453
00:20:22,830 --> 00:20:19,179
great so and we're trying to that's what

454
00:20:25,740 --> 00:20:22,840
we're going to try to do next so add

455
00:20:28,740 --> 00:20:25,750
more parameters to our models so maybe

456
00:20:32,909 --> 00:20:28,750
things like wind so when I talk about

457
00:20:34,740 --> 00:20:32,919
wind things so radial outflows I call

458
00:20:39,029 --> 00:20:34,750
outflows and anything that's horizontal

459
00:20:41,159 --> 00:20:39,039
I call wind and so maybe if we if we add

460
00:20:43,980 --> 00:20:41,169
that kind of horizontal motion we can

461
00:20:46,470 --> 00:20:43,990
reproduce these strong blue shifts or if

462
00:20:48,810 --> 00:20:46,480
we make atmospheric profiles different

463
00:20:51,299 --> 00:20:48,820
on the day side versus nighttime which

464
00:20:53,940 --> 00:20:51,309
is not unrealistic to expect I think we

465
00:20:55,470 --> 00:20:53,950
might have a better fit to the data but

466
00:20:57,470 --> 00:20:55,480
in order to start adding more and more

467
00:21:00,000 --> 00:20:57,480
parameters we first needed to make a

468
00:21:02,210 --> 00:21:00,010
radiative transfer code much faster and

469
00:21:04,890 --> 00:21:02,220
this was the work that was done by my

470
00:21:07,710 --> 00:21:04,900
REE student this summer Caleb Kurata

471
00:21:10,200 --> 00:21:07,720
he's an undergrad from Maryland and she

472
00:21:11,880 --> 00:21:10,210
did really an outstanding job at making

473
00:21:14,010 --> 00:21:11,890
the code faster and more efficient and

474
00:21:16,020 --> 00:21:14,020
so now we think we can really start

475
00:21:18,750 --> 00:21:16,030
adding more parameters and try to match

476
00:21:21,210 --> 00:21:18,760
the entire time series of spectra

477
00:21:23,039 --> 00:21:21,220
instead of just the average and transit

478
00:21:25,529 --> 00:21:23,049
spectrum and see what we can learn about

479
00:21:29,070 --> 00:21:25,539
the additional physical and dynamics of

480
00:21:31,890 --> 00:21:29,080
the atmosphere but even if that proves

481
00:21:33,659 --> 00:21:31,900
not to be enough we can always look for

482
00:21:36,590 --> 00:21:33,669
more complicated and complex structures

483
00:21:40,560 --> 00:21:36,600
so there has been a lot of work done on

484
00:21:42,330 --> 00:21:40,570
trying to model planetary winds and

485
00:21:44,789 --> 00:21:42,340
Celer winds and how they might interact

486
00:21:48,870 --> 00:21:44,799
some what kind of geometries they might

487
00:21:51,270 --> 00:21:48,880
form so in this work from 2015 and also

488
00:21:53,100 --> 00:21:51,280
John McCain's work from earlier this

489
00:21:55,770 --> 00:21:53,110
year and I'm sorry I forgot to mention

490
00:21:58,110 --> 00:21:55,780
that he has bolster above this so

491
00:22:01,230 --> 00:21:58,120
basically the material that escapes the

492
00:22:03,480 --> 00:22:01,240
planet might form a leading arm that

493
00:22:06,570 --> 00:22:03,490
kind of goes to the star and causes his

494
00:22:08,549 --> 00:22:06,580
redshift and then the trailing arm that

495
00:22:11,789 --> 00:22:08,559
is kind of blown away by stellar winds

496
00:22:13,860 --> 00:22:11,799
and you call these blue shift perhaps so

497
00:22:15,899 --> 00:22:13,870
this is work that I'm currently doing

498
00:22:17,520 --> 00:22:15,909
with Morgan MacLeod who's an Einstein

499
00:22:18,710 --> 00:22:17,530
fellow at the CF faith

500
00:22:21,330 --> 00:22:18,720
we're trying to create these 3d

501
00:22:23,790 --> 00:22:21,340
hydrodynamic simulations of planetary

502
00:22:26,160 --> 00:22:23,800
outflows for the moment we're just

503
00:22:27,420 --> 00:22:26,170
putting them in basically by hand and

504
00:22:30,750 --> 00:22:27,430
trying to see what happens to their

505
00:22:32,250 --> 00:22:30,760
geometry and dynamics and we're yet not

506
00:22:34,260 --> 00:22:32,260
trying to launch them really self

507
00:22:37,170 --> 00:22:34,270
consistently but that is something that

508
00:22:39,600 --> 00:22:37,180
we'll try to do in the future but yeah

509
00:22:42,870 --> 00:22:39,610
this is one way that we can try to get

510
00:22:45,240 --> 00:22:42,880
as these shifts by basically doing ray

511
00:22:48,840 --> 00:22:45,250
tracing through this material and see

512
00:22:52,950 --> 00:22:48,850
what kind of shifts we get so I kind of

513
00:22:55,680 --> 00:22:52,960
to wrap up this part so we can look for

514
00:22:57,930 --> 00:22:55,690
evidence of atmospheric escape if we

515
00:23:00,300 --> 00:22:57,940
observe this extended atmospheres of

516
00:23:02,490 --> 00:23:00,310
exoplanets so even though technically

517
00:23:04,710 --> 00:23:02,500
we're not probing the gas that's outside

518
00:23:06,840 --> 00:23:04,720
of the Roche radius so it's not like I'm

519
00:23:08,610 --> 00:23:06,850
and also where you actually see this

520
00:23:11,730 --> 00:23:08,620
tail of material that has already

521
00:23:14,370 --> 00:23:11,740
escaped in helium were probably probing

522
00:23:17,130 --> 00:23:14,380
these regions inside the Roche radius

523
00:23:19,650 --> 00:23:17,140
but if we can study dynamics of this

524
00:23:22,200 --> 00:23:19,660
material to sufficient detail and find

525
00:23:24,360 --> 00:23:22,210
evidence that there are these radial

526
00:23:26,070 --> 00:23:24,370
outflows then basically that tells us

527
00:23:29,010 --> 00:23:26,080
that this gas has to go somewhere so it

528
00:23:31,290 --> 00:23:29,020
has to escape at some point and I think

529
00:23:33,480 --> 00:23:31,300
the best way to move forward is to try

530
00:23:35,430 --> 00:23:33,490
to combine not just observations in the

531
00:23:38,070 --> 00:23:35,440
helium line but other lines that might

532
00:23:41,250 --> 00:23:38,080
be probing slightly different regions of

533
00:23:44,100 --> 00:23:41,260
the wind like H alpha or sodium doublet

534
00:23:46,050 --> 00:23:44,110
line and kind of use the information

535
00:23:48,570 --> 00:23:46,060
from all these lines to create a full

536
00:23:52,350 --> 00:23:48,580
picture of these planetary outflows and

537
00:23:54,750 --> 00:23:52,360
this is a some work that's been shown on

538
00:23:56,850 --> 00:23:54,760
Monday at posters by Julia and Ahriman

539
00:23:59,460 --> 00:23:56,860
and I hope you got a chance to see them

540
00:24:01,920 --> 00:23:59,470
they've been looking at sodium and H all

541
00:24:04,040 --> 00:24:01,930
fine they basically also see evidence of

542
00:24:06,330 --> 00:24:04,050
these outflows

543
00:24:09,750 --> 00:24:06,340
alright so people often ask me where

544
00:24:12,510 --> 00:24:09,760
should we look for these planets so here

545
00:24:15,270 --> 00:24:12,520
this plot shows basically the strength

546
00:24:17,820 --> 00:24:15,280
of the helium feature as a function of

547
00:24:20,040 --> 00:24:17,830
extreme UV flux from the host star and

548
00:24:22,980 --> 00:24:20,050
it's really interesting to see that all

549
00:24:25,650 --> 00:24:22,990
the detection is shown in blue are here

550
00:24:26,970 --> 00:24:25,660
and these are non detection and also

551
00:24:29,640 --> 00:24:26,980
some Atlanta attractions that are not on

552
00:24:31,230 --> 00:24:29,650
the plot so there seems there isn't

553
00:24:33,960 --> 00:24:31,240
things that

554
00:24:36,300 --> 00:24:33,970
whether or not we see helium and a

555
00:24:39,300 --> 00:24:36,310
planet might be related to how much XE

556
00:24:40,830 --> 00:24:39,310
reflux we see from the start but I think

557
00:24:43,110 --> 00:24:40,840
it's also really interesting to look at

558
00:24:46,340 --> 00:24:43,120
the spectral type types of these host

559
00:24:48,930 --> 00:24:46,350
stars for all of these planets that have

560
00:24:52,290 --> 00:24:48,940
strongest signals orbit around K type

561
00:24:57,210 --> 00:24:52,300
stars whereas these non detection czar

562
00:24:58,860 --> 00:24:57,220
around a M G and L as well so maybe this

563
00:25:03,750 --> 00:24:58,870
could be telling us something about how

564
00:25:05,880 --> 00:25:03,760
helium is excited and how how the

565
00:25:07,680 --> 00:25:05,890
strength of the signal depends on the

566
00:25:12,780 --> 00:25:07,690
properties of the host star

567
00:25:14,460 --> 00:25:12,790
so in this plot I basically show most of

568
00:25:16,260 --> 00:25:14,470
the processes that are involved in

569
00:25:18,750 --> 00:25:16,270
populating and depopulating the

570
00:25:20,400 --> 00:25:18,760
metastable helium level and for the sake

571
00:25:22,560 --> 00:25:20,410
of this talk you can ignore all of them

572
00:25:25,140 --> 00:25:22,570
except this thing in purple line which

573
00:25:27,740 --> 00:25:25,150
shows that the pink line is the main

574
00:25:29,730 --> 00:25:27,750
populating mechanism which is just

575
00:25:32,850 --> 00:25:29,740
fertilization of the ground state and

576
00:25:37,020 --> 00:25:32,860
then recombination and this is photons

577
00:25:38,790 --> 00:25:37,030
that live here and the popular you can

578
00:25:40,830 --> 00:25:38,800
be populate the helium triplet through

579
00:25:43,590 --> 00:25:40,840
direct for photo ionization from these

580
00:25:48,300 --> 00:25:43,600
photons which are here and basically I

581
00:25:49,860 --> 00:25:48,310
think the one of the main important key

582
00:25:52,680 --> 00:25:49,870
features to look in a stellar spectrum

583
00:25:55,080 --> 00:25:52,690
is the ratio of flux in this band and

584
00:25:58,290 --> 00:25:55,090
this band because this will tell us how

585
00:26:00,510 --> 00:25:58,300
the helium levels are populated and

586
00:26:04,580 --> 00:26:00,520
basically by analyzing that we see that

587
00:26:08,670 --> 00:26:04,590
K stars seem to be more most favorable

588
00:26:10,350 --> 00:26:08,680
more favorable than other types so

589
00:26:12,630 --> 00:26:10,360
basically just proving the same point if

590
00:26:15,120 --> 00:26:12,640
we increase the x-ray flux we increase

591
00:26:20,670 --> 00:26:15,130
the helium population level and if we

592
00:26:22,530 --> 00:26:20,680
decrease this mid UV flux we can again

593
00:26:25,560 --> 00:26:22,540
increase helium so basically what does

594
00:26:27,750 --> 00:26:25,570
this tell us it tells us that the

595
00:26:29,460 --> 00:26:27,760
whether or not we see helium signal will

596
00:26:32,250 --> 00:26:29,470
not only depend on the properties of the

597
00:26:33,630 --> 00:26:32,260
planetary atmosphere but also will

598
00:26:35,340 --> 00:26:33,640
depend on the properties of the host

599
00:26:37,560 --> 00:26:35,350
star so we need to take that into

600
00:26:41,190 --> 00:26:37,570
account when we make any interpretations

601
00:26:44,460 --> 00:26:41,200
of whether or not we've seen helium in

602
00:26:46,500 --> 00:26:44,470
some planets or not and also it's often

603
00:26:48,480 --> 00:26:46,510
miss I just want to point out that this

604
00:26:51,810 --> 00:26:48,490
doesn't mean that we absolutely cannot

605
00:26:53,940 --> 00:26:51,820
see helium around other stars and K

606
00:26:55,770 --> 00:26:53,950
stars we can if the conditions are right

607
00:26:58,980 --> 00:26:55,780
it's just that the conditions are most

608
00:27:00,690 --> 00:26:58,990
easily met around K stars and I'll just

609
00:27:02,880 --> 00:27:00,700
skip this slide it just shows that it's

610
00:27:05,330 --> 00:27:02,890
fairly important to have good models of

611
00:27:09,300 --> 00:27:05,340
XUV flux if we want to have reliable

612
00:27:10,680 --> 00:27:09,310
modeling and this is my summary I will

613
00:27:12,420 --> 00:27:10,690
just leave it up there because I'm out

614
00:27:29,550 --> 00:27:12,430
of time so thank you for your attention

615
00:27:31,860 --> 00:27:29,560
please state your name and affiliation

616
00:28:00,630 --> 00:27:31,870
even if people know you some people

617
00:28:05,490 --> 00:28:02,420
[Music]

618
00:28:08,600 --> 00:28:05,500
particular said you shot this the shift

619
00:28:10,980 --> 00:28:08,610
from from red to blue have you have you

620
00:28:12,930 --> 00:28:10,990
investigated how this would look like in

621
00:28:14,250 --> 00:28:12,940
the stellar frame just to make sure that

622
00:28:15,810 --> 00:28:14,260
it's not some kind of star signal that

623
00:28:18,090 --> 00:28:15,820
this you yeah yeah

624
00:28:21,390 --> 00:28:18,100
I haven't back up slides that I can

625
00:28:22,950 --> 00:28:21,400
maybe show you later because moves to an

626
00:28:25,320 --> 00:28:22,960
original presentation yeah it's fine

627
00:28:26,910 --> 00:28:25,330
yeah we did this is something with we're

628
00:28:28,740 --> 00:28:26,920
still checking but I think we did test

629
00:28:31,830 --> 00:28:28,750
and for example if you compare to that

630
00:28:34,800 --> 00:28:31,840
strong silicon line that's right to the

631
00:28:37,590 --> 00:28:34,810
blue in the search it just stays fixed

632
00:28:39,390 --> 00:28:37,600
and you can see by even by I in picks or

633
00:28:41,640 --> 00:28:39,400
when you plot pixels that the hilum line

634
00:28:57,430 --> 00:28:41,650
tab moves yeah I'd be happy to show you

635
00:29:11,919 --> 00:29:07,690
microphone yeah you know thanks Antonia

636
00:29:13,749 --> 00:29:11,929
and the result from GJ 1214 and was a

637
00:29:15,970 --> 00:29:13,759
non detection how much of that is

638
00:29:17,440 --> 00:29:15,980
affected by having clouds like do you

639
00:29:21,430 --> 00:29:17,450
expect that that feature to be strongly

640
00:29:23,710 --> 00:29:21,440
neutered as well yeah the GJ 1214 is

641
00:29:25,539 --> 00:29:23,720
actually very it was lower the wall

642
00:29:27,340 --> 00:29:25,549
spectral resolution so I think it's

643
00:29:32,850 --> 00:29:27,350
still not completely relaxed I would say

644
00:29:37,659 --> 00:29:32,860
but there has been some recent work

645
00:29:39,490 --> 00:29:37,669
doing simulations but I can't forget

646
00:29:41,499 --> 00:29:39,500
Venice forget the authors now but

647
00:29:43,749 --> 00:29:41,509
suggest that actually helium should

648
00:29:45,490 --> 00:29:43,759
extend out beyond that so it shouldn't

649
00:29:59,560 --> 00:29:45,500
mouth should not be an issue for the

650
00:30:01,419 --> 00:29:59,570
okay great talk Ted Temasek you Chicago

651
00:30:03,460 --> 00:30:01,429
so when you were showing the winds is

652
00:30:05,860 --> 00:30:03,470
kind of following up on Beorn's question

653
00:30:07,419 --> 00:30:05,870
were you removing the planetary rotation

654
00:30:09,580 --> 00:30:07,429
when you put it the wind speeds because

655
00:30:09,940 --> 00:30:09,590
they were quite fast sorry can you

656
00:30:11,409 --> 00:30:09,950
repeat

657
00:30:15,639 --> 00:30:11,419
were you removing the planetary rotation

658
00:30:17,769 --> 00:30:15,649
further I included in modeling so it's

659
00:30:19,330 --> 00:30:17,779
when I when I make my theoretical

660
00:30:32,139 --> 00:30:19,340
spectra includes like tidally locked

661
00:30:34,659 --> 00:30:32,149
rotations oh yeah included the question

662
00:30:36,190 --> 00:30:34,669
came up if you check if it's a stellar

663
00:30:37,629 --> 00:30:36,200
residual and you also looked into the

664
00:30:39,639 --> 00:30:37,639
rest of the McLoughlin effect because it

665
00:30:43,149 --> 00:30:39,649
would be bigger for a very extended

666
00:30:45,580 --> 00:30:43,159
atmosphere and but I thought about it

667
00:30:47,320 --> 00:30:45,590
but WASC 107 is very the star is a very

668
00:30:49,149 --> 00:30:47,330
slow door fader it's like I think

669
00:30:52,090 --> 00:30:49,159
Messiah is like two and a half

670
00:30:54,789 --> 00:30:52,100
kilometers per second and it's there's a

671
00:30:57,850 --> 00:30:54,799
paper by Diane Winne that suggests that

672
00:31:00,149 --> 00:30:57,860
it's it has very high obliquity so even

673
00:31:04,299 --> 00:31:00,159
on top of that small rotations probably

674
00:31:07,539 --> 00:31:04,309
transiting at high obliquity so I don't

675
00:31:09,730 --> 00:31:07,549
think we can explain 10 km/s shifts with

676
00:31:10,670 --> 00:31:09,740
with Ruster McLaughlin's but okay thank

677
00:31:14,750 --> 00:31:10,680
you