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[Music]

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good evening everyone thank you for

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coming out this is the first session of

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Astro biology graduate conference 2017

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it's very exciting Thank You Brett for

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helping to leave the the charge on this

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one what I'm going to introduce to you

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guys today is a session that has been

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leveling lovingly called the building

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planets and listening to the songs of

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their peoples session and so what I'm

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going to do is introduce you to the

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schedule there is a slight change

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Amelio is actually currently in transit

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so his talk is going to be bumped to

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just before the winning PWR presentation

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so Ryan Loomis if you're in the audience

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if you can come get Mike DUP yeah that's

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you

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so Ryan's gonna take it off as soon as

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we get done with this intro talk but as

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you can see we're kind of all over the

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map here we've got some SETI we've got a

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couple of talks about disks and then

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we've got planets orbiting white dwarves

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and then we've got some education with

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the coherent content storyline on

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exoplanets now it seems like these are

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all very disparate ideas but I want to

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assure you that in the grand scheme of

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astrobiology no idea is too far-fetched

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to find a home and as you can see here

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on this lovely diagram of this entire

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session the universe and you know the

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galaxies and the solar system starts off

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as some nebulous cloud condenses down to

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a disk we get a star that star lives for

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some 10 billion years or so and then

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explodes and dies and leaves us with a

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white dwarf now just to put all of the

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talks into some sort of context we think

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that somewhere in here we might find

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some intelligent life form that may want

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to communicate with us if you know we're

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cool and don't panic the idea here is

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that you also need to worry about how

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disks form and evolve because that's how

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planets form and their host stars around

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their host stars

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and we're also going to about white

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tours which is the the sort of terminal

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end point for low mass stellar objects

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throughout the universe and then we're

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also going to figure out how you might

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teach this stuff how you might introduce

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it to an audience either your peers or

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more likely an audience of middle school

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to high school students and so just to

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put some names on here this is sort of

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the breakdown for who's going to be

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talking about what now because I

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uploaded this before the last minute

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schedule change it's going to be

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slightly out of order so I'm going to

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introduce you to the SETI talk first

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which is based on some work that's being

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funded through the break through listen

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project which has devoted about a

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hundred million dollars over the next

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ten years to try to find aliens now the

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way they're doing it with modern

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technologies is for example 100-meter a

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Green Bank telescope which is as I

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understand the largest steerable radio

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antenna in the world the largest the

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largest steerable structure in the world

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that's crazy

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and then some smaller ones but who cares

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about those so those are the current

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technologies no we don't care about you

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so those are what we're currently using

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to try to find these radio signals that

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other intelligent species might be

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sending out we're also using something

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called LOFAR which the low-frequency

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array that's looking for similar

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transmissions from other types of

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objects and together these current

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technologies are really trying to reach

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out and touch something like the nearest

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hundred thousand stars in the system and

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if this works okay so we're going to

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take a small tour just to give you an

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idea of the sense of the scale of this

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SETI search so obviously this is the Sun

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it's a pretty cool Sun you might say and

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then that's the solar system to give you

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a sense of scale I'm not entirely sure

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obviously voyager is the farthest flung

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human innovation in the history of the

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earth as far as we know and so that's

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one light year you can see that the Oort

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cloud is just a tiny little speck in the

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middle of the screen of this I'm sorry

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the Oort cloud is a speck now because

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you're starting to look at some of our

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nearest stars come on one more so that's

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sort of the local neighborhood these are

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some of the the brightest stars in the

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sky generally and some of the dimmest

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ones too because you can't actually see

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them with the naked eye in some cases

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and then we pause it here this is the

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nearest hundred thousand stars in the

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sky that's a lot of places to to knock

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bread

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I got it okay

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so like I said they're looking at

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something like the nearest hundred

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thousand stars which is a lot of real

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estate and not just with the current

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technologies but also with several new

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arrays that are coming online in the

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next couple years or tens of years for

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example in the next generation Very

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Large Array or the Square Kilometre

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Array these are very large radio

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telescope arrays and the one I believe

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we're going to hear about today

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assuming that Emilio actually does make

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his travel plans is going to be some

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work from the low-frequency array low

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farm to of the talks in this session are

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going to be about discs so here's a

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lovely JPL rendering of what we might

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see if we were actually able to get

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close enough to one of these discs

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thankfully we don't have to rely just on

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JPL animations we can actually observe

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these out in the the wild this is a

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Chell tower II and Alma image and this

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is Elias 227 which shows that lovely

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spiral arm structure that we tend to

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associate with galaxies but it also

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shows up in smaller scale features like

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protoplanetary disks now one of the

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really cool things about these disks is

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that they tend to be exceptionally

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short-lived and this is showing you how

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many stars at what age have a disk for

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example so most stars that are fairly

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young a few million years old 80 or 90

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percent of them tend to have disks and

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then as you get past between 15 and 20

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million years most of the disks have

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gone away so a lot of the planet

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building action occurs in an incredibly

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short amount of time and there's a lot

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of complexity a lot of richness in how

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these disks evolve and then we're going

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to hear about two different aspects of

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disks in terms of visualizing them and

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then modeling them with these magneto

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hydrodynamic models that couple the

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stellar magnetic fields with disk

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interactions to figure out how you might

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initiate either gap formation or

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rich location in material that you can

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form planets with it like you can see

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the gaps here and the bands so gaps can

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either be cleared by planets that are

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forming in that region or they can be

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cleared by magnetic field interactions

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with the disc and so there there's a lot

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of really rich material in here that you

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can sort of delve into and and you get

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different chunks of that disc depending

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on what you observe it with now to go to

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one of the other talks in our session we

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want to figure out where white dwarves

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live and so this is the famous

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hertzsprung-russell diagram this is the

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main sequence here the Sun is sitting

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prettily here it's about a g2 star now

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as the Sun evolves it will evolve into

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the Giants class and then it'll shoot

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over here and then down onto the white

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dwarf track because it's a smaller star

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anything about you know a few solar

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masses tends to evolve down onto the

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white dwarf tract anything larger than

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that turns into a black hole which you

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know it's harder to observe or not as

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interesting at least for the context of

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the session we're talking about today

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and white dwarves can start off really

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really really hot like tens of thousands

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of degrees even up to one literature

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survey suggested up to about a hundred

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and fifty thousand degrees when they

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start out but they cool relatively

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rapidly in that initial phase and then

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they they sit around the you know five

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to ten thousand degree range for a few

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billion years as they cool off towards

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that background temperature of the

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galaxy and one of the things you can see

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here is that for a white dwarf at a

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similar temperature to the Sun and as a

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similar blackbody spectrum so you might

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expect that it would be kind of like

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living under the Sun and that just shows

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you the evolution of habitable zone time

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is marching upwards in this diagram and

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the distance to the host star is here in

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this case it's the white dwarf and so I

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just want to point out that this tick

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mark here 0.005 au is equivalent to one

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solar radius so that means that if you

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had a main-sequence solar type star and

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you had a terrestrial planet litter

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we parked in its envelope and then that

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star exploded in that terrestrial planet

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managed to survive it would find itself

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in the the habitable zone of a white

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dwarf after about a billion years and so

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there's a lot of complexity and how you

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find planets well not in how you find

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plants but how you get planets to be

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that close to their parent stars after

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such a cataclysmic evolutionary event

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for them and just to point out that

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these white dwarves are incredibly small

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as well so they're bright small and

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that's why they're habitable zones are

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so close in and one of the last talks

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we're going to be hearing about today is

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the Danny Barringer's talk about the

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coherent content storyline which

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involves some elements from education

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including the claimed evidence and

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reasoning strategy where you make a

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claim about some result of an

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investigation and then you try to back

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it up and then you tie together those

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claims in that evidence and this is all

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part of the next generation science

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standards which looks at connecting

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scientific practices with core ideas and

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then sort of tying that into a broader

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context with these cross-cutting ideas

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these cross-cutting concepts and the

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cohesive content storyline is all about

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making sure that when you're telling

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someone a story about a scientific event

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or concept that the context in which you

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provide them that information all feeds

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into that main point and all feeds into

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that rational discussion about that

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concept and the after the session but

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it's sort of in the same session we're

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going to hear a little bit more about

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the proposal writing retreat which is a

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workshop that brings together a number

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of students it's actually 25

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participants this year in 9 different

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groups that wrote proposals that range

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from spectral polarimetry catalog for

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exoplanet surface characterization to

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the characterization of the solid geyser

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effluent and approach for Enceladus so

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lots of crazy stuff that's being

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suggested as potentially interesting for

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your

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peers and we'll hear more from that from

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Becky I believe later and so with that I

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would be happy to take any potential

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questions you might have

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first off the answer is going to be 42

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and then if you don't know or didn't

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catch it and that goes for this whole

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conference ask all right so I'll take

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questions I'll bring in Mike so you can

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be heard by the streamers Brent you get

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to be co-chairing um and then Bradley

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can be dealer yeah oh yeah you mentioned

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the SETI project there hundred thousand

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stars does anyone have like a rough

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estimation of how many like planets

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within that set

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I'm sure someone does but I think it's a

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large enough sample that it's going to

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follow the occurrence rates from Kepler

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so you know M star planets did you have

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a you have a question so it's going to

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follow Kepler statistics so you know

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about roughly 1/3 of the M stars will

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have planets and then you know roughly a

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quarter of the g-type stars will have

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plants so so special plants in our

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habitable zones I should say scale

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magnitude order of magnitude they're

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probably going to be anywhere between 10

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and 30 thousand terrestrial planets and

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avalible zones where on the nearest

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hundred thousand stars cool thank you