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[Music]

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as much as we'd love science to just be

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about science it's unfortunately kind of

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mostly about money um and so it's really

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important I think to get some exposure

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to how you get money and how you move

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from there so you may or may not have

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that opportunity in your graduate career

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and so what we have is we have a little

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retreat a proposal writing retreat every

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year before AB grad con where you get

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the opportunity to work in a small group

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and put together a complete proposal so

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this year we had everybody answer roses

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solicitation call so that's the main

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NASA sort of single Pi grant

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solicitation every year but there's a

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lot of different calls within that broad

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roses perspective and so this year as

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Sonny was saying we had 25 participants

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in nine groups of two or three people

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and they had a little over two days to

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write a full grant which includes

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obviously the science proposal but also

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the budget the data management plan you

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have to think about things like overhead

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and fringe benefits sort of all the

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nitty-gritty stuff that you may or may

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not see um in your day to day life as a

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graduate student and it uh so people

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signed up to work really hard this

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weekend but it's not just hard work

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people have fun too and it wasn't just

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the organizers um and so it's it's a

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really great opportunity and I would

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like to encourage anyone to apply next

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year it's I I mean talk to the people

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who went can everybody who went stand up

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actually so it was a significant portion

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this year so um talk to them see if they

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think it was worthwhile I think it's

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worthwhile and I didn't encourage you to

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apply next year as well part of the

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process is writing the proposal but we

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also have

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we'll turn their proposals in and then

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everyone gets the opportunity to review

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other proposals and then the next day

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after everyone's reviewed the proposals

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we go through and we do a mock review

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session where you go through and get to

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go through the process of receiving

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feedback and talking in sort of a panel

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situation um so that's also a really

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useful thing and from that we pick we

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rank the proposals and we well on yeah

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Frank the proposals and pick and so we

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had three proposals that um sort of

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stood out and so we had group 2 which

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was the spectra Poehler spectra of

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polarimetry catalog for expedited

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surface characterization and UV

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radiation the double-edged sword in

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prebiotic chemistry but our winners who

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will be hearing from next where the

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exploring radiation effects on the

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surface of Europa and implications for

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prebiotic molecules synthesis and

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distribution one of the things we

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encouraged is budgeting reasonably um

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but you'll see that as long as you

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budget reasonably within what you

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propose to do we gave a little

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flexibility on the size of the overall

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budget ah but we'll be hearing from them

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[Applause]

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all right hi everybody

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so I'm Zoe I'm currently at Harvard

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University in the Department of

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astronomy I'm Deidre I am a second year

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grad student at Georgia Tech I'm Chris

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I'm a PhD student here at UVA steady

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astrochemistry all right and like we

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just said we're going to be discussing

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our proposal exploring a radiation

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effects on the surface of Europa and

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modifications in implications for

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prebiotic molecules synthesis and

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distribution which we submitted to the

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e4 habitable worlds program okay so the

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overall science objectives for our

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proposal here basically the main point

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we want to determine is the identity and

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abundance of various chemicals in the

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subsurface ocean on Europa

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so Europa has a pretty harsh a radiation

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environment so we were going to first

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with our first science objective s1

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model the radiation driven non

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equilibrium chemistry on the surface ice

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and then we're also going to be able to

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attract the abundances of different

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molecules that are formed on the icy

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shell as a function of time but these

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molecules on the surface of Europa are

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not very useful and then of themselves

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for prebiotic chemistry so then we want

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to model how many of those get down to

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the surface or to the subsurface ocean

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so we use convective ice transport

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models to get the transport rates for

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these complex organic molecules and then

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finally our third science objective is

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to understand what further chemical

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reactions can occur once you get these

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molecules into the aqueous phase so in

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aqueous phase you could have such

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reactions as hydrolysis decomposition or

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further chemical Network reactions

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polymerization this will affect the

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chemistry that ultimately occurs

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so we're seeding molecules from the icy

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surface and then getting them down into

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the aqueous ocean and seeing what

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happens out of there so the relevance of

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our research has been echoed throughout

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many NASA documents the decadal survey

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the astrobiology roadmap the current

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science plan the science Mission

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Directorate but most importantly the

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roses solicitation for habitable world

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some of the major touchstones for

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habitable worlds are covered under our

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research specifically determining

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processes and conditions that create and

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maintain habitable environments and the

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search for habitable environments to

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explore the possibility of

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extraterrestrial extant life right so in

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europa you've got two things which are

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good for making prebiotic molecules also

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destroying them but you've got ice

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you've also got irradiation what can you

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do with that well there are tons of

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experiments out there where you take

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mixed ices and you've been barred them

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with radiation and you can make cool

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things things is cool or cooler than

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glycine so yeah so normally we think of

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radiation as being something which

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breaks things down and that's certainly

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true but it can also make things so one

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of our technical objectives in fact t1

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is to constrain a model that we have to

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simulate the chemistry of a and

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irradiated ice so that we can model

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which kinds of molecules would form in

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your open ice analogs so just to

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convince you that there's plenty of a

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radiation to go around for everyone on

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Europa here we have a table showing a

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solar system body and the amount of REMS

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per day that you would expect there now

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REMS per day tells you roughly how much

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you'd have to worry about starting to

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glow the more REMS per day the more

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glowy that you would get in some

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alternate reality so take a look at

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Earth so the average fairly low good for

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us even the max is still insignificant

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compared to the REMS per day experienced

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on Europa so there's plenty of radiation

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and of course it's Europa so there's

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plenty of ice so you mix the two and you

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can make potentially some very cool

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things all right and then once we have

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those chemical models from the first

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technical objectives we also want to

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verify these and explore some more

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parameter space with our second

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technical objective so for this we're

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going to build and test an ice

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irradiation apparatus

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so here we're going to be able to

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deposit various types of Isis so

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different chemical compositions to try

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to mimic the Europen ice or variations

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to that then we also want to have

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several radiation setups here to really

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mimic the radiation environment on the

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surface of Europa

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this would include protons electrons and

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photons over a wide range of energies so

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instead of just being able to radiate

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say at one wavelength through photons or

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one energy for protons our setup is

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going to be able to scan a range of

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energies in order to be able to really

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explore parameters faced and see how the

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radiation environment on Europa would

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actually drive certain chemistry

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processes so then on the other side what

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are we going to be able to do to detect

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these molecules so the detection

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equipment will include something like

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mass spectrometry and then a variety of

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absorption instrumentation including UV

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vis and IR so here we'll be able to

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irradiated types of Isis deposit at

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different deposition temperatures with

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various irradiation sources and

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combinations of these at a variety of

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energies and then be able to detect the

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outputs and characterize them okay so

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our third technical objective is to

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study the stability of the complex

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organic molecules that are made on the

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surface by the irradiation chemistry and

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to see if they can survive the perilous

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journey from the outer brittle cold

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shell where they're made as I mentioned

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subject to significant irradiation all

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the way down mmm and they gets abducted

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in this sort of surface plate tectonic

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activity that brings them down into the

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warmer convecting ice layer from there

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they can move over time from the top of

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the convecting ice layer down to the ice

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water interface and at the ice water

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interface get introduced to the

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subsurface ocean so what we want to know

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is can these molecules survive

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chemically in the time it takes to go

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from the surface to the subsurface ocean

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so we can run additional models to do

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that and this leads to our fourth

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technical objective is that we want to

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look at the existing solid state

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convective models try to run them

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see what we get for the rates of

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transport from the surface again down to

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the ice liquid interface see if we know

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how much is surviving and the rate it

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takes to get from the top to the bottom

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of the ice shell then we can say how

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many of these complex organic molecules

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are being introduced to again the far

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more biologically friendly environment

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of the subsurface ocean our final

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technically objectively to look at the

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polymerization and decomposition

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composition rates of complex organic

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molecules and in the Europan subsurface

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ocean this can be done using the many

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analytical facilities available to us at

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Georgia Tech's core facilities so we

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have two different mass spec core

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facilities we have spectroscopy

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equipment and we also have a bio

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analytical facility and that's where we

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intend to look at these synthesized

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comms so our budget is rather generous

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but we think that it is understandable

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given the scope of our research it will

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be split into three different sections

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for each of the Co eyes at each of the

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institutions

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we plan to hire three graduate students

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in addition to a researcher and we need

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our salaries and we also require a to

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buy a supercomputer we need the ISO

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radiation equipment we need time on our

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core facility equipment as well yes so

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for the low low low low price of two

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mega dollars and sixty mega cents you

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too can have a fully functioning

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radiation chemistry lab / group so just

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to summarize and bring it all together

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we feel that our proposal is definitely

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closely tied to the habitable habitable

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worlds goal of determining the processes

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and conditions that create and maintain

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habitable environments the surface of

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radiation could create the complex

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molecules that can then be introduced

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into a more habitable environment so

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again we feel this is connected there

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and once again walking through what we

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hope to do we hope to simulate and

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experiment surface irradiation processes

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to see what you can form we're not

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coming into this with any expectations

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we want to look at the kinds of complex

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molecules you can make using appropriate

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ice analogs and then we want to see if

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they can survive over geophysical

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timescales to be transported from the

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brittle surface to the subsurface ocean

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and then we want to see what kinds of

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neat and more prebiotic chemistry they

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can do in the aqueous subsurface ocean

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so just to finish of course the

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background is a very nice Jacques

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Cousteau's undersea world of Europen

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exobiology and you see anticipating

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perhaps some life and the hydrothermal

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vent analog to what we see here on earth

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and that's certainly one place where you

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might find life at the sort of liminal

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zone between two different phases of a

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planet between the solid phase and the

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liquid phase but if you look at the top

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there's the ice water layer and so we're

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proposing that perhaps that could be

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also very interesting in terms of

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astrobiology if you look at environments

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like Antarctica

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these are also very important

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environments for life and for the

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ecosystem there so thank you very much

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okay do have any questions quick

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questions okay yeah so now that you have

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this nice experimental setup that's

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really expensive I assume you can use it

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to study other possibly habitable worlds

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what's next after Europa yeah so that's

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a great point this isn't just a one and

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done deal this isn't you know a million

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dollars for only three years of research

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this can be used for long periods after

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that so the next main thing that comes

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to mind is to do this for comment Isis

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or interstellar ices interstellar dust

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particles that kind of thing so there

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you have a larger variety of the

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composition of those materials so you

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might look at more co2 ices or Co ices

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and really see what you can get on the

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interstellar phase chemistry happening

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or on comet surfaces so what is a sort

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of hand waving estimate for the

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subduction rate from the surface and I

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guess as a secondary follow-up do you

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expect the mass loading from the top

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down to be comparable to the bottom

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these are excellent questions I am NOT a

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geologist so I have no idea what the

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answer is but if you fund us we will

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okay just a quick piggyback on that last

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comment there are some people that

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suggest that the Europen crust is

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actually quite thick which will you have

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this problem of rigidity and lack of

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conductive flow convective flow excuse

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me versus if you have rapid turnover

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then you also have a more oxidizing

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potentially a more oxidizing environment

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which changes your chemistry's hold it

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how would you address those two

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scenarios well so that would come into

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play in terms of the rate at which the

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species would come from the brittle

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surface to whatever the aqueous

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environment would be so we would try to

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use the models in there are existing

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models and they take into account not

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only the convective ice model of the

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open ice structure but also the more

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brittle other type in which case I

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believe you probably have faster arrival

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of the complex organics produced on the

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surface on the subsurface ocean if it

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didn't have to convect all the way

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through so there's a thinner ice model