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[Music]

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first of all I like to thank the

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opportunity to talk so this is my first

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time talking outside Brazil and maybe my

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English not very good but please forgive

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me um my name is Eleni I'm from Brazil

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and I'm finishing my master's right now

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and starting my PhD next month

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so this work I'm going to be showing you

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is my Master's work and it's about the

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information of molecules entitled

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atmosphere um first of all I like to

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start on telling you what's really

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interesting about Titan because many

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people don't know all the features so

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first of all we see the evidence of

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lakes really on the surface of the Moon

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just like the earth but um it they're

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basically formed by methane and organic

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molecules and you're gonna see that a

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little bit later as well we also see um

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volcanism just like the earth but some

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people believe there's a ocean of

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ammonia and water under the surface so

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maybe this is a way of um giving water

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to the surface after of the moon and my

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favorite part is right here that Titan

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is the only place in the solar system

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besides our planet that can is able to

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build complex and organic molecules so

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when I say complex I'm talking about

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molecules which are and which have at

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least six or more atoms and organic

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they're basically formed by carbon and

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hydrogen and we're gonna see some one

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because that's where all this nitrogen

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and oxygen so um a little bit um about

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the chemistry in Titan so just like he

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said before me we basically start

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everything with this two

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main molecules so these are nitrogen and

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methane so nitrogen is about 94 95

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percent in the atmosphere and methane is

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like basically the rest of it so this is

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where the chemistry all starts we have

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two main influences which are the solar

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radiation and basically in the u

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ultraviolet or extreme ultraviolet and

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we have another source of particles

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especially energetic particles like ions

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and electrons which come from Saturn

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because of its heavy because of its

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heavy magnetic field so there are some

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particles coming from Titans

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magnetosphere that's what we call and

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then these particles are going to be the

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second main influencer to start breaking

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these molecules and their chemistry

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starts so basically with these two main

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influences this remain Malik's are going

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to break and we're gonna start building

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more complex molecules from them so

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basically we have two main things called

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the dissociation and the ionization of

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these two molecules so this is the these

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are the two main processes that will

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create the the bigger molecules in Titan

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so just like the earth we can separate

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the the atmosphere in different layers

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but just to show you that here in the

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thermistors like the upper atmosphere

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about a thousand to 1400 um these are

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the two main models that I showed you

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methane and nitrogen so this area is

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where it out is where I'm going to start

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so when we go down the atmosphere we see

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the creation of more complex and organic

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molecules we can see here compounds made

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by carbon and hydrogen so when they're

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from they get heavier and then they go

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down the atmosphere so here in the

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lowest part this that

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the second lowest part dissatisfied we

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see something we call aerosol haze layer

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which are these organic molecules that

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start to condense and are gluten aid and

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if they form Isis and solid particles in

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the atmosphere so this which we call the

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haze layer is the reason we see when we

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observe Titan we see this very dense

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very thick kind of orange yellow

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atmosphere it's because of these

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particles these organic particles right

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here so I'm gonna talk now about my work

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this is me okay and these are my two

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advisors from from Brazil as well from

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the federal University of Rio de Janeiro

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so us three we got um we this is one of

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my advisors and she had this work with

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the southern offers where they developed

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a model to simulate atmosphere but not

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for Titan they develop it to study hot

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Jupiters so they're near my two advisors

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me a bunch of advisers we were like oh

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let's try this let's try this chemical

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model for something different for

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something that's more terrestrial maybe

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and which we know a little bit more

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because hot Jupiters are not really well

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known so we try this this chemical model

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for Titan but the problem was we can

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only work with the upper atmosphere

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that's not really a problem for us

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because as I showed you the main

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chemistry works a is really in the upper

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atmosphere in the thermosphere part but

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so basically this is why I studied

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Titans upper atmosphere so above a

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thousand kilometers and in the in the

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upper atmosphere we have these features

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is very important in my work which is

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called the atmospheric escape so some

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molecules are going to just

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escape the atmosphere as it happens here

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on the river as it happens in hot

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Jupiters and other atmospheres so this

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is how by this mechanism we're going to

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to analyze the formation of molecules in

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the atmosphere so um basically the first

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step of my work was we selected a bunch

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of species which we know from the

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literature that were in Titan's

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atmosphere so I went to a database

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called the you missed I don't know if

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any one who uses it

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it's database for interstellar molecules

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we had to adapt it to to put this

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molecules in Titan atmosphere and what

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after we selected this these compounds

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we here in the database we got all the

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reactions that these compounds go

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through so here for example this is a

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methane which is one of the main

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products of reactions in Titan so here

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in the database we have all the

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reactions that will happen with a thing

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for information and for destruction as

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well so we got all these reactions we

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got all day out there constants and we

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put it on the equations and this is um

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this is basically the word so the last

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part is we put all that reaction in

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equations in continuation continuity

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equations and we use the program to

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solve that so basically the continuity

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equation for the molecules is basically

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this one which is one molecule so we

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have one separate equation for each

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molecule we have like a 100 molecules or

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something so the reactions go right here

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this is a reactions product right and

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this is the loss rate but our um our

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mother our mother was um only

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dimensional and stationary so we didn't

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considered time so this goes to zero

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actually and then two to

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but this molecules in my work I had to

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put some previous profiles for the main

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molecules so I put the profiles for

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nitrogen and for methane

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I also use the profile for hydrogen

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molecular hydrogen because it's the main

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molecule that's going to escape the

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atmosphere and sit for working with

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upper atmosphere

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I used hydrogen as well these two

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profiles are from this work in 2008 so

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this is our result I'm gonna show you

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the main marks we found basically these

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three main molecules which are called

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acetylene ethylene anything are the

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three main products my reactions in

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Titan's atmosphere so this is their

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abundances and this is the altitude it's

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in the horizontal but you pretend like

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the Titan is here and the altitude is

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going that way so these are the three

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and this remaining molecules we found by

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that products by that reaction sorry and

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these are basically the hyper

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hydrocarbon molecules so we also find

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molecules with oxygen but I didn't

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mention oxygen before because it's not

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it's initially not in Titan's atmosphere

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it actually comes from Enceladus so it

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has a inflow of oxygen especially

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especially oxygen ions in the atmosphere

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so we also we can also see some some

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oxygen bearing molecules here and we see

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co which is basically um I guess the

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fourth may molecule in in the atmosphere

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and it's really stable because its

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contents temperature is really cold so

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it basically doesn't condense in fact in

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the atmosphere and the best part for me

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is that we also found nitrogen bearing

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molecules which is important for life

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and stuff so this is the main molecule

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we found which is hydrogen cyanide is

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one of the basic molecules we can find

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in the interstellar medium and we're

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found different molecules as well so we

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found some we found some complex

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molecules which is great for us because

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you can see this like anywhere else in

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the solar system so we found this one

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for examples for pure nitrile we found

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Osetra nitrile and this CN was settling

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to me and yes that's a pretty great

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result for us um another thing we did in

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our work was try to show the difference

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between considering the energetic

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particles that come from Saturn's

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magnetosphere so we tried to run the

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model with and without this influence of

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energetic particles so I show you here

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some molecules and some ions and we can

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see if um these these direct ones are

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without the magnetospheric influence and

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the solid ones are considering the

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magnetospheric influence so we basically

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discovered that this influence is

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especially in small molecules and ions

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so the biggest molecules we found they

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were not affected by this this

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magnetospheric energetic particles so

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basically this comes this concludes my

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work

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we found the abundances the simulated

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abundances for compounds with carbon

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hydrogen oxygen and nitrogen we got um a

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pretty good simulation considering we

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didn't consider other mechanisms like

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the haze formation which is lower in the

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atmosphere we just consider the upper

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atmosphere for this work and we also

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found some visible effects of the

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influence of Saturn's magnetosphere so

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for the future what I want to do with

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this work maybe not me but some other

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student we want to try to include more

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molecules in this model especially maybe

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sulfur and phosphorus molecules which

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are also really important if we want to

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find life somewhere we want to include

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the Collins and his formations so we

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want to to run the model for all the

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atmosphere not just the upper atmosphere

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and we want to try to do some lab

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experiments trying to simulate that

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really in a chamber with all the

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molecules we found and see if that could

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develop anything else or anything

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different we from we found in the

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computer in the computer computer model

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this is basically my wor solo I'm open

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to any questions now if you have them

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thank you thank you very much for that

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thank you very much for the talk we have

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any questions we got time for maybe one

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or two so the question is about

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methodology from your ears to your

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modeling okay so we when we had to put

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each reaction in this continuous

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irritation equation we have for example

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from the database we have the reactions

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constants constants and then we put on

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we put on this continuity equation but

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we adhere factor to to consider the

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folks from system and the flux from the

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energetic particles no sorry it's

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actually here so we have here the flux

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factor then we add another constant here

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to to consider this influence so we did

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that for two different things for the UV

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sunlight and then for the Saturn

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energetic particles I just um I went

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through this part because it's it's the

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[Music]

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with it with it we actually um yes we're

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considered elected to it all uniform but

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we actually know in fact that Murphy we

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have wind and circulation of convection

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circulation this is something else we

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could put in the model but it's a really

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difficult thing to do so since we did

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consider but is here in the upper

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atmosphere they're not really in

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like

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yeah we considered they're all going to

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- they're going to be uniform basically

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as I said in the latitude and everywhere

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else but we just considered a

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one-dimensional model so this is we

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actually work with the altitude

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dimension I'm sorry to put it in the

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horizontally this is not very this is

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very weird for me but the model works

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like this so we only considered this

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direction the other directions were not