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[Music]

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hello as Miguel said

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um

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my name is Marshall and I'm an NPP

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fellow at JPL Caltech and I work with

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Morgan cable and Brianna Henderson and I

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do most of my experimental work at

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Caltech and Paul asimov's lab but

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because this is a conference of

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literally graduate students and postdocs

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I wanted to talk about the planetary

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science summer school program which is a

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program for graduate students and

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postdocs to teach you all how to help

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Mission design for planetary missions

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actually happens and to learn the

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process and so I'm going to be

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presenting

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the mission that my team and I developed

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during the PSS

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in which the majority of the framework

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for the mission was developed back in

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2021 and that we iterated on since then

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the astrobiology exploration at

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Enceladus or X for short and I'm going

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to preface this by saying that this is

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an Unholy amount of information to

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distill into a dozen slides and so uh I

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did my best unfortunately I can't go

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into a lot of detail with these slides

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but if you have any questions about the

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science ask a question if you don't want

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to ask a question come find me I'd love

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to be stoked to talk about this stuff

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Okay so

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I'm sure you guys are familiar with

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Enceladus at this point

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um but that thing is in Solace it's one

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of uh Saturn's moons and it's it's

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relatively pretty small it's only about

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500 uh kilometers in diameter but

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there's some super cool stuff going on

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even though it's it's this tiny little

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thing that stuff coming out of the

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bottom of Enceladus

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um is a continuous plume that's formed

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over the South polar Terrain

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and so if we zoom in a little bit closer

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these are images from Cassini and though

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it's not actually blue like that that's

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in false color but that's just to show

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you where these um fractures are

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and the plume is sourced from those

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fractures

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um that all combines to form a

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continuous plume over the South polar

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terrain and we have really strong

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evidence from some of the measurements

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by Cassini that this plume is directly

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sourced from a subsurface Global liquid

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water ocean

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and so this presents a unique

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opportunity we're unique in our solar

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system to sample the contents of a

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subsurface ocean in situ using uh

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multi-flyby or an Orbiter Mission

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architecture

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and we have some rough compositional

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information of the plume uh from Cassini

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using the inms or the ion and neutral

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Mass spectrometer and the cosmic dust

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analyzer and so

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um in the plume gas we see water

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um small hydrocarbons some simple and

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complex Organics and this is a paper

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from

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the weight at all paper back in 2006

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from the inms data but if we look at

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plume grains we see that they're

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waterized but um we see a lot of

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different salts but in addition to that

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and I I think a previous talk hit on

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this a little bit we see silicon Nano

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grains and that's really important

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because based on what we know the only

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way that these silicon nanoparticles

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could be produced within this size range

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are high temperature hydrothermal

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reactions and that's huge from a

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habitability standpoint and in addition

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to this

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looking at the CDA data that Cosmic dust

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analyzer we see evidence not direct

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detection because of the the

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instrumental capabilities we had at the

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time this is like 80s technology

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but we see strong evidence for

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macromolecular organic compounds

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and so there's this complex organic

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chemistry going on that we don't really

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understand and we don't know what's

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going on there but like something's

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happening and so we need to figure out

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what's up

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and so with that being said we have

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liquid water we have a geothermal source

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of feed via the high temperature

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hydrothermal reactions

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[Music]

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um

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essentially all the chemical building

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blocks for Life as we know it they're

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present

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um sulfur hasn't been published yet but

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it has been detected in the greens it

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should be published in the next year or

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so so with all of this

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in mind could Enceladus

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Harbor life

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we thought it would be sick to develop a

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mission concept that would be capable of

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finding out and so just a brief overview

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of our mission architecture it's be it

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multiply by Mission but you're orbiting

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Saturn and do multiple flybysmen zeldas

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and we would require 30 flybys for our

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science and would launch in 2033 and

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after a nine-year cruise phase and a

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one-year pump down phase we would enter

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four years of science operations

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where we would directly search for

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biosignatures through n-situ chemical

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compositional analysis of the plume and

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contextualize these in-situ measurement

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in-situ measurements through a

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synergistic combination of geophysical

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and geomorphological investigations

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aimed at also assessing the habitability

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of Enceladus over geologic time

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and we would do this using a mass

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spectrometer a high resolution camera

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and just a high gain antenna so three it

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well two and a half instruments because

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the antenna you use for radio

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communications

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and so just briefly to talk about how

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before I dive into the science

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objectives how these objectives were

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formulated

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um NASA

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doesn't like

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as much when people just when they're

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developing missions to like take this

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instrument okay we have a sick

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instrument what kind of science can we

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do with it instead

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um we were taught and we were informed

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that NASA prefers that you first start

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by answering or by asking questions like

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what do we not know about Enceladus what

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do we need to know to ask more questions

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and so that's what we started by doing

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and if you do that if you start from the

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science questions and what you're

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interested in and what you want to find

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out the rest of it follows pretty

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logically and so say we want to find out

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this thing okay what do we need to

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measure to figure that thing out okay

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then you have your measurement

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requirements and then at what levels do

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we need to measure this there you have

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like further established measurement

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requirements well how do we make these

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measurements and then you select your

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instruments and then so on and so forth

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and so it just logically flows from it's

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called left to right approach

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and so I'll talk a little bit about our

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science objectives of course the first

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which is to determine if the molecular

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and isotopic distributions uh within the

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plume are a result of biological

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activity or abiotic chemical processing

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and we would do this just with your

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usual suspects amino acids fatty acids

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and plume grains and um by assessing

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isotopic fractionation in um in the

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plume gas and we would do this just

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using a mass spectrometer and if you

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have any questions about Mass specs or

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instrument selection please ask a

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question or find me later I'd love to

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talk about that

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and the second of our objectives is to

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determine whether Enceladus is in

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thermal equilibrium and is therefore

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capable of sustaining an ocean over

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geologic time scales and this is

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essentially just a heat balance equation

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we want to know how much being how much

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heat is being input to Enceladus through

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tidal dissipation from Saturn and how

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much heat is being emitted by Enceladus

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through like um conductive heat loss and

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you can

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actually determine the heat being

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generated

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looking at tidal dissipation from Saturn

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and you can do this using orbital

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migration rates so you could look at

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where Enceladus is at in its orbital

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phase relative to What was seen by

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Cassini to see how the orbital migration

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happens and

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uh from that you could calculate a tidal

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dissipation quality factor and you can

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determine the heat being emitted by

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measuring ice shell thickness which is a

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proxy for the heat loss and you can do

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that using a gravity science

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measurements

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the third of our objective objectives

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is looking at plume formation mechanisms

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to determine whether the plume material

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is being delivered to the surface via

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open crevice boiling or explosive

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cryovolcanic-like eruptions and we

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expect there to be differences in the

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morphology of the vents at the surface

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that are expressed in each scenario and

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you could

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actually sort of tease out how these

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plumes are being formed by high

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resolution imaging of the vents so for

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an open crevice model we expect there to

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be

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vent width variations in response to

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Tidal forcing throughout enceladus's

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orbital phase and for an open crevice

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model we expect these vent width

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variations to be consistent along the

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strike of the vent

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and so by taking multiple high

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resolution images of a single vent

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throughout enceladus's orbital phase and

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looking at vent width variations we can

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determine if that were the case whereas

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for a purely cryovolcanic eruptive model

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we expect these vent width variations to

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be restricted to the immediate vicinity

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of the vent

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and so we could sort of tease out the

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relative contribution of each of these

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models to plume formation

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and then our fourth and final science

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objective

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is to determine if the geologic activity

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that uh is modifying the South polar

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terrain like we see in all those awesome

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images if it's influenced other regions

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in the past over geologic time

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we would do this by looking at two

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things both crater infilling and

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elliptical crater orientations because

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if you look at the depth diameter ratios

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of craters around the South polar

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terrain they're pretty shallow compared

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to the rest of the the crater population

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because of all that plume Fallout that's

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infilling the craters and so we see

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really shallow craters around there

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but if you look at the global crater

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population like typically

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um they have a pretty well defined depth

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diameter ratio and so if we were to look

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at survey the global crater population

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and find an area around Enceladus where

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we see anomalously infilled craters that

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could be evidence that there was past

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plume activity and another thing that we

282
00:10:41,090 --> 00:10:38,880
would look at uh are elliptical crater

283
00:10:42,889 --> 00:10:41,100
orientations to see if there could have

284
00:10:45,650 --> 00:10:42,899
been any eye shell reorientation in the

285
00:10:47,150 --> 00:10:45,660
past because given a preferential

286
00:10:48,949 --> 00:10:47,160
velocity vector and the impactor

287
00:10:51,590 --> 00:10:48,959
population and a small enough impact

288
00:10:53,990 --> 00:10:51,600
angle below about 15 degrees elliptical

289
00:10:55,430 --> 00:10:54,000
craters are formed and so like given a

290
00:10:58,130 --> 00:10:55,440
preferential velocity Vector we expect

291
00:10:58,850 --> 00:10:58,140
to see mostly East-West

292
00:11:02,030 --> 00:10:58,860
um

293
00:11:04,430 --> 00:11:02,040
uh oriented elliptical craters

294
00:11:08,509 --> 00:11:04,440
and so if we were to survey the crater

295
00:11:10,250 --> 00:11:08,519
population and see a shift in the

296
00:11:12,590 --> 00:11:10,260
orientation of these elliptical craters

297
00:11:14,449 --> 00:11:12,600
that is like relatively consistent we

298
00:11:17,630 --> 00:11:14,459
could infer past eye shell reorientation

299
00:11:24,170 --> 00:11:20,150
and so for the mission trajectory

300
00:11:26,329 --> 00:11:24,180
um briefly we'd use a Venus Earth Earth

301
00:11:30,790 --> 00:11:26,339
Venus Earth Earth Earth Jupiter gravity

302
00:11:32,990 --> 00:11:30,800
assist where we would do we do a a

303
00:11:34,610 --> 00:11:33,000
slingshot around Venus and then a couple

304
00:11:36,230 --> 00:11:34,620
orbits around Earth and then slingshot

305
00:11:37,910 --> 00:11:36,240
out to the Jupiter system and then use

306
00:11:40,790 --> 00:11:37,920
Jupiter's gravity to slingshot out into

307
00:11:43,370 --> 00:11:40,800
the Saturn system but

308
00:11:45,710 --> 00:11:43,380
getting out to Saturn isn't a problem

309
00:11:48,050 --> 00:11:45,720
it's slowing down that's the problem

310
00:11:50,990 --> 00:11:48,060
because you're going like 15 20

311
00:11:52,490 --> 00:11:51,000
kilometers a second and so after Saturn

312
00:11:55,250 --> 00:11:52,500
orbital insertion

313
00:11:57,410 --> 00:11:55,260
we do a one-year pump down phase and

314
00:11:59,870 --> 00:11:57,420
using multiple use multiple flybys of

315
00:12:03,230 --> 00:11:59,880
Titan using Titan's gravity to reduce

316
00:12:05,990 --> 00:12:03,240
the spacecraft velocity and tailor the

317
00:12:08,030 --> 00:12:06,000
inclination and altitude such that we

318
00:12:10,670 --> 00:12:08,040
could Target and sell at us properly for

319
00:12:12,050 --> 00:12:10,680
our flybys and then after that enter a

320
00:12:13,550 --> 00:12:12,060
four-year tour phase where we would

321
00:12:17,449 --> 00:12:13,560
conduct all of our science operations

322
00:12:20,269 --> 00:12:17,459
that would consist of 30 flybys at least

323
00:12:22,430 --> 00:12:20,279
and this is this uh requirement is

324
00:12:25,190 --> 00:12:22,440
driven primarily by our gravity science

325
00:12:26,990 --> 00:12:25,200
measurements that we need to make and

326
00:12:30,769 --> 00:12:27,000
the surface mapping would require a

327
00:12:34,250 --> 00:12:30,779
total of 22 flybys not necessarily 22

328
00:12:37,730 --> 00:12:34,260
flybys total dedicated surface mapping

329
00:12:41,090 --> 00:12:37,740
but the data downlink would require 22

330
00:12:43,069 --> 00:12:41,100
flybys um and so a minimum of five

331
00:12:45,170 --> 00:12:43,079
flybys at low altitudes as well for

332
00:12:47,389 --> 00:12:45,180
event imagery and Institute Bloom

333
00:12:50,269 --> 00:12:47,399
analyzes

334
00:12:52,069 --> 00:12:50,279
so keyword to key takeaway uh installed

335
00:12:54,009 --> 00:12:52,079
is a sick it's super awesome there's a

336
00:12:56,690 --> 00:12:54,019
lot of really cool stuff going on there

337
00:12:58,730 --> 00:12:56,700
and we would

338
00:13:01,069 --> 00:12:58,740
see what's going on there by looking at

339
00:13:04,009 --> 00:13:01,079
plume composition heat balance the

340
00:13:07,670 --> 00:13:04,019
different event formation mechanisms and

341
00:13:09,590 --> 00:13:07,680
what the surface of Enceladus can tell

342
00:13:11,329 --> 00:13:09,600
us about its past

343
00:13:13,389 --> 00:13:11,339
and this is important because in the

344
00:13:16,129 --> 00:13:13,399
most recent decadal survey

345
00:13:19,370 --> 00:13:16,139
they specifically call out a New

346
00:13:21,829 --> 00:13:19,380
Frontiers mission to Enceladus using a

347
00:13:23,389 --> 00:13:21,839
multi-flyby mission architecture and so

348
00:13:25,370 --> 00:13:23,399
there's so many outstanding questions

349
00:13:26,930 --> 00:13:25,380
that we just we just don't know about

350
00:13:30,110 --> 00:13:26,940
what's going on in Enceladus and we need

351
00:13:32,629 --> 00:13:30,120
to go back to figure out what's going on

352
00:13:36,230 --> 00:13:32,639
so as promised a little talk about PSS

353
00:13:38,170 --> 00:13:36,240
this is my team that I worked with and

354
00:13:40,610 --> 00:13:38,180
they're the most

355
00:13:41,870 --> 00:13:40,620
absurdly brilliant group of people that

356
00:13:43,190 --> 00:13:41,880
I've ever had the pleasure of working

357
00:13:44,509 --> 00:13:43,200
with

358
00:13:46,310 --> 00:13:44,519
um they're incredible I'm still friends

359
00:13:48,590 --> 00:13:46,320
with many of them now

360
00:13:50,509 --> 00:13:48,600
um and so I I'd like to talk a little

361
00:13:52,910 --> 00:13:50,519
bit about the PSS

362
00:13:55,129 --> 00:13:52,920
um it's uh it's not really as much of a

363
00:13:57,949 --> 00:13:55,139
summer school as it is a rigorous

364
00:14:01,370 --> 00:13:57,959
Mission design program where they teach

365
00:14:03,050 --> 00:14:01,380
you how to actually formulate a mission

366
00:14:05,090 --> 00:14:03,060
um and the deadlines pass for this year

367
00:14:07,310 --> 00:14:05,100
but it's it's it's competitive you have

368
00:14:09,050 --> 00:14:07,320
to apply for it and they take 18 people

369
00:14:10,910 --> 00:14:09,060
per cohort

370
00:14:12,829 --> 00:14:10,920
um but you get to work with literally

371
00:14:15,050 --> 00:14:12,839
the best in the business

372
00:14:17,449 --> 00:14:15,060
um you're mentored by people that are on

373
00:14:19,430 --> 00:14:17,459
like Europa Clipper Mars sample return

374
00:14:22,730 --> 00:14:19,440
all that kind of stuff and in the last

375
00:14:26,509 --> 00:14:22,740
week you get to work one-on-one and are

376
00:14:30,410 --> 00:14:26,519
mentored by a member of NASA's uh

377
00:14:32,449 --> 00:14:30,420
Advanced project design team uh TMax

378
00:14:34,730 --> 00:14:32,459
they're literally the best at what they

379
00:14:37,190 --> 00:14:34,740
do formulating missions and you've

380
00:14:37,910 --> 00:14:37,200
learned so much and it's incredible

381
00:14:40,310 --> 00:14:37,920
um

382
00:14:42,230 --> 00:14:40,320
if you have any questions please come

383
00:14:43,670 --> 00:14:42,240
find me ask here or if you don't want to

384
00:14:46,490 --> 00:14:43,680
ask a question in front of a bunch of

385
00:14:49,490 --> 00:14:46,500
people come find me talk to me

386
00:14:50,930 --> 00:14:49,500
um I knew when I first like was thinking

387
00:14:52,009 --> 00:14:50,940
about doing it I was like oh my God I

388
00:14:54,050 --> 00:14:52,019
don't know anything about Mission design

389
00:14:55,910 --> 00:14:54,060
how am I going to do this but everybody

390
00:14:57,410 --> 00:14:55,920
else in my court thought the exact same

391
00:14:59,210 --> 00:14:57,420
thing so you don't need to be an expert

392
00:15:01,670 --> 00:14:59,220
in Mission design you just need to be

393
00:15:03,290 --> 00:15:01,680
interested and enthusiastic about doing

394
00:15:05,930 --> 00:15:03,300
this stuff and this is the the most

395
00:15:08,269 --> 00:15:05,940
incredible experience I've had of my

396
00:15:11,150 --> 00:15:08,279
professional career so I would highly

397
00:15:13,730 --> 00:15:11,160
highly recommend this program to anybody

398
00:15:22,910 --> 00:15:13,740
interested in Mission design

399
00:15:22,920 --> 00:15:30,889
any questions

400
00:15:35,329 --> 00:15:34,550
hi Michael I'm from UCSD just up the

401
00:15:37,970 --> 00:15:35,339
hill

402
00:15:41,629 --> 00:15:37,980
um I was wondering

403
00:15:43,069 --> 00:15:41,639
is there like how quickly or is it

404
00:15:47,689 --> 00:15:43,079
plooming like is it gonna run out of

405
00:15:53,750 --> 00:15:49,730
um oh

406
00:15:56,090 --> 00:15:53,760
it's been active for I mean Enceladus is

407
00:15:58,910 --> 00:15:56,100
anywhere between like 100 million and

408
00:16:01,670 --> 00:15:58,920
over one two billion years old

409
00:16:05,090 --> 00:16:01,680
um and it's been like the e-ring around

410
00:16:06,650 --> 00:16:05,100
Saturn is composed mostly of Enceladus

411
00:16:08,870 --> 00:16:06,660
plume materials so we know it's been

412
00:16:11,990 --> 00:16:08,880
around for a very very long time

413
00:16:13,550 --> 00:16:12,000
and we also know that the ocean is is a

414
00:16:15,170 --> 00:16:13,560
quite large

415
00:16:18,410 --> 00:16:15,180
um and makes up a pretty significant

416
00:16:21,829 --> 00:16:18,420
portion of the the mass of the Moon so I

417
00:16:24,110 --> 00:16:21,839
I there's a not any evidence as far as

418
00:16:25,910 --> 00:16:24,120
I'm concerned or as far as I know uh

419
00:16:37,610 --> 00:16:25,920
that it's running out anytime soon and

420
00:16:41,629 --> 00:16:39,350
I'm curious

421
00:16:43,910 --> 00:16:41,639
um does this program kind of have a

422
00:16:45,470 --> 00:16:43,920
component where you assess the costs of

423
00:16:50,949 --> 00:16:45,480
certain missions and sort of optimize

424
00:16:55,670 --> 00:16:53,810
that's the it's like the entire last

425
00:16:58,249 --> 00:16:55,680
week is like the so the New Frontiers

426
00:17:00,470 --> 00:16:58,259
five cost cap is 900 million and it

427
00:17:04,250 --> 00:17:00,480
takes like 700 million to take a piece

428
00:17:06,890 --> 00:17:04,260
of cardboard to Enceladus and so

429
00:17:08,449 --> 00:17:06,900
and so yeah that's a huge part of it and

430
00:17:10,610 --> 00:17:08,459
that's like a huge part of like working

431
00:17:13,189 --> 00:17:10,620
with TMax is to try and do rapid

432
00:17:15,890 --> 00:17:13,199
iterations of your your mission concept

433
00:17:18,230 --> 00:17:15,900
to see what you can do and what trade

434
00:17:21,590 --> 00:17:18,240
space you can explore to fall with under

435
00:17:23,390 --> 00:17:21,600
the cost cap because the problem isn't

436
00:17:25,130 --> 00:17:23,400
like finding all the science to do

437
00:17:27,370 --> 00:17:25,140
because like there's so much science you

438
00:17:31,130 --> 00:17:27,380
can do it's finding

439
00:17:33,950 --> 00:17:31,140
what it's doing the most science for the

440
00:17:37,370 --> 00:17:33,960
least money and so unfortunately that is

441
00:17:38,450 --> 00:17:37,380
a massive part of mission design and

442
00:17:48,289 --> 00:17:38,460
formulation

443
00:17:54,049 --> 00:17:51,230
hi uh Colin Robinson uh very man

444
00:17:55,310 --> 00:17:54,059
University I I was just wondering uh I

445
00:17:58,190 --> 00:17:55,320
know one of the big

446
00:18:00,650 --> 00:17:58,200
hindrances to uh sampling Organics from

447
00:18:03,289 --> 00:18:00,660
blooms and Enceladus is uh destruction

448
00:18:05,570 --> 00:18:03,299
of Organics because in the sampling

449
00:18:06,950 --> 00:18:05,580
processes right because of velocity and

450
00:18:09,110 --> 00:18:06,960
you just

451
00:18:10,669 --> 00:18:09,120
go you know at high speeds through the

452
00:18:12,110 --> 00:18:10,679
bloom with like a cup to pick up all

453
00:18:14,330 --> 00:18:12,120
that stuff lots of Organics are just

454
00:18:16,669 --> 00:18:14,340
gonna be obliterated so what steps were

455
00:18:19,610 --> 00:18:16,679
you guys thinking of taking to eliminate

456
00:18:21,230 --> 00:18:19,620
destruction of Bio signatures

457
00:18:22,190 --> 00:18:21,240
thank you so much for asking that

458
00:18:22,730 --> 00:18:22,200
question

459
00:18:25,070 --> 00:18:22,740
um

460
00:18:26,930 --> 00:18:25,080
I actually that's the research that I'm

461
00:18:30,169 --> 00:18:26,940
doing at Caltech is we're simulating

462
00:18:30,950 --> 00:18:30,179
hyper velocity impacts of eye screens

463
00:18:32,750 --> 00:18:30,960
um

464
00:18:35,750 --> 00:18:32,760
using impact ionization mass

465
00:18:37,430 --> 00:18:35,760
spectrometry and we're the only lab in

466
00:18:39,230 --> 00:18:37,440
the world that can do that at the moment

467
00:18:41,630 --> 00:18:39,240
they can actually simulate a

468
00:18:43,610 --> 00:18:41,640
distribution of I well I don't want to

469
00:18:45,590 --> 00:18:43,620
get i'll nerd out too much come find me

470
00:18:48,130 --> 00:18:45,600
to talk about that after after this if

471
00:18:51,590 --> 00:18:48,140
you want but to answer your question yes

472
00:18:54,710 --> 00:18:51,600
there is a velocity regime where you

473
00:18:56,270 --> 00:18:54,720
have both efficient ionization assuming

474
00:18:58,490 --> 00:18:56,280
you're using an impact ionization Mass

475
00:19:00,110 --> 00:18:58,500
spectrometer for analysis of plume

476
00:19:02,990 --> 00:19:00,120
grains which is pretty necessary at this

477
00:19:05,870 --> 00:19:03,000
stage yes there is a velocity regime

478
00:19:08,330 --> 00:19:05,880
that you have efficient ionization and

479
00:19:10,730 --> 00:19:08,340
molecular survivability for a range of

480
00:19:13,190 --> 00:19:10,740
of compound classes and the

481
00:19:15,470 --> 00:19:13,200
survivability velocity range

482
00:19:18,049 --> 00:19:15,480
um is depends on molecular functionality

483
00:19:19,850 --> 00:19:18,059
but it's somewhere between four and six

484
00:19:22,310 --> 00:19:19,860
kilometers per second it is like the

485
00:19:24,049 --> 00:19:22,320
Goldilocks zone that you wanna that you

486
00:19:26,750 --> 00:19:24,059
want to sample at so yes that's a

487
00:19:28,430 --> 00:19:26,760
fantastic question and that is a problem

488
00:19:30,830 --> 00:19:28,440
that a lot of very smart people are

489
00:19:32,330 --> 00:19:30,840
trying to solve right now in in terms of

490
00:19:34,730 --> 00:19:32,340
that speed four to six kilometers per

491
00:19:36,169 --> 00:19:34,740
second uh is that fast enough to be able

492
00:19:38,930 --> 00:19:36,179
to stay out of the gravitational pull of

493
00:19:40,130 --> 00:19:38,940
Enceladus okay yeah Enceladus does it

494
00:19:42,650 --> 00:19:40,140
there's not very much gravity there

495
00:19:47,990 --> 00:19:42,660
exactly that's tiny yeah thank you no

496
00:19:55,270 --> 00:19:51,529
uh hi I'm over for Veronica from Cornell

497
00:20:01,810 --> 00:19:59,210
but whether it's like a open for

498
00:20:04,789 --> 00:20:01,820
fracture for purposes uh cryova

499
00:20:08,529 --> 00:20:04,799
volcanism is that going to

500
00:20:13,669 --> 00:20:08,539
um impact the types of uh biosis

501
00:20:14,690 --> 00:20:13,679
signatures that uh could be detected

502
00:20:17,810 --> 00:20:14,700
yes

503
00:20:18,529 --> 00:20:17,820
very much so that's a fantastic question

504
00:20:20,450 --> 00:20:18,539
um

505
00:20:23,150 --> 00:20:20,460
in each case

506
00:20:26,810 --> 00:20:23,160
um the mechanism of plume formation

507
00:20:28,130 --> 00:20:26,820
that's under underlying the surface

508
00:20:29,690 --> 00:20:28,140
um

509
00:20:32,990 --> 00:20:29,700
I'm trying to think of the best way to

510
00:20:36,110 --> 00:20:33,000
say it but the way the grains are formed

511
00:20:37,909 --> 00:20:36,120
actually strongly influences the

512
00:20:40,490 --> 00:20:37,919
composition of the grains because you

513
00:20:43,250 --> 00:20:40,500
have homogeneous nucleation where if you

514
00:20:45,529 --> 00:20:43,260
just have like water that just freezes

515
00:20:48,049 --> 00:20:45,539
and is is shot out in the like the open

516
00:20:49,970 --> 00:20:48,059
crevice boiling situation

517
00:20:52,190 --> 00:20:49,980
um where you have uh

518
00:20:54,049 --> 00:20:52,200
a heterogeneous nucleation where you

519
00:20:58,310 --> 00:20:54,059
have well I don't want to get too much

520
00:21:00,770 --> 00:20:58,320
in the weeds but but uh yes um for a an

521
00:21:01,789 --> 00:21:00,780
explosive cryovolcanic scenario like you

522
00:21:05,090 --> 00:21:01,799
mentioned

523
00:21:07,010 --> 00:21:05,100
um we wouldn't see very many

524
00:21:09,529 --> 00:21:07,020
um compositional differences from grain

525
00:21:11,570 --> 00:21:09,539
to grain whereas for the open crevice

526
00:21:14,810 --> 00:21:11,580
boiling scenario due to the different

527
00:21:17,270 --> 00:21:14,820
ice cream nucleation processes that that

528
00:21:19,190 --> 00:21:17,280
can occur you would see very distinct

529
00:21:21,890 --> 00:21:19,200
compositional differences in the grains

530
00:21:23,050 --> 00:21:21,900
and we see that in the CDA data that's

531
00:21:23,690 --> 00:21:23,060
where all those the

532
00:21:25,190 --> 00:21:23,700
[Music]

533
00:21:27,169 --> 00:21:25,200
um

534
00:21:28,370 --> 00:21:27,179
evidence for those Organics that I was

535
00:21:31,190 --> 00:21:28,380
talking about before those complex

536
00:21:34,370 --> 00:21:31,200
Organics that comes from Ice grains that

537
00:21:37,149 --> 00:21:34,380
are composed primarily of an organic

538
00:21:40,850 --> 00:21:37,159
phase that were formed very likely

539
00:21:42,289 --> 00:21:40,860
through open crevice boiling and so

540
00:21:45,590 --> 00:21:42,299
um I guess that's a long answer to

541
00:21:49,250 --> 00:21:45,600
saying yes that it very much matters

542
00:21:53,330 --> 00:21:51,649
okay our lunch delivery is running a

543
00:22:00,370 --> 00:21:53,340
little late so we have time for another

544
00:22:04,310 --> 00:22:02,390
thanks Marshall I've heard this talk

545
00:22:06,289 --> 00:22:04,320
many times you're welcome and every time

546
00:22:07,730 --> 00:22:06,299
and every time it's enjoyable and every

547
00:22:10,610 --> 00:22:07,740
time I feel like I ask the question

548
00:22:12,169 --> 00:22:10,620
about uh what kind of mass spectrometer

549
00:22:15,649 --> 00:22:12,179
are you going to include what kind of

550
00:22:18,169 --> 00:22:15,659
resolution or msms capabilities do you

551
00:22:20,149 --> 00:22:18,179
need to detect bioseignatures get

552
00:22:22,789 --> 00:22:20,159
isotopic information

553
00:22:25,130 --> 00:22:22,799
get through matrices of the salt grains

554
00:22:27,529 --> 00:22:25,140
crystals thank you you gave me an excuse

555
00:22:30,049 --> 00:22:27,539
to talk about that now

556
00:22:33,710 --> 00:22:30,059
um so for for the the

557
00:22:37,549 --> 00:22:33,720
gas the plume gas you need some sort of

558
00:22:39,710 --> 00:22:37,559
like uh qitms or like Mass specs type

559
00:22:41,090 --> 00:22:39,720
instrument that I'm sure you're familiar

560
00:22:44,210 --> 00:22:41,100
with that stuff

561
00:22:46,130 --> 00:22:44,220
um but where you need to be able to like

562
00:22:48,770 --> 00:22:46,140
have a sample Inlet where you take gas

563
00:22:50,210 --> 00:22:48,780
in and then you you determine the the

564
00:22:53,510 --> 00:22:50,220
composition of that and that's really

565
00:22:55,130 --> 00:22:53,520
necessary for uh assessing isotopic

566
00:22:56,390 --> 00:22:55,140
fractionation

567
00:22:59,270 --> 00:22:56,400
um because those typically have very

568
00:23:01,010 --> 00:22:59,280
high mass resolution which you need for

569
00:23:04,669 --> 00:23:01,020
looking at different isotope logs and

570
00:23:07,909 --> 00:23:04,679
things whereas for the plume grains

571
00:23:10,010 --> 00:23:07,919
um a lot of dust detectors don't have

572
00:23:11,750 --> 00:23:10,020
the same mass resolution

573
00:23:13,789 --> 00:23:11,760
um just due to the the way the

574
00:23:16,070 --> 00:23:13,799
instruments are designed and but you

575
00:23:18,830 --> 00:23:16,080
need information about the ice cream

576
00:23:21,169 --> 00:23:18,840
composition because of all the cool

577
00:23:22,909 --> 00:23:21,179
stuff is in the grains and the lower the

578
00:23:25,850 --> 00:23:22,919
bigger the grains are the lower the

579
00:23:28,070 --> 00:23:25,860
velocity the or the lower the altitude

580
00:23:31,070 --> 00:23:28,080
uh the more interesting the grin

581
00:23:34,070 --> 00:23:31,080
composition is and so you need

582
00:23:35,870 --> 00:23:34,080
in theory you could just use one to

583
00:23:37,610 --> 00:23:35,880
answer your question like a mass specs

584
00:23:39,529 --> 00:23:37,620
type instrument

585
00:23:41,210 --> 00:23:39,539
um where when I for those people that

586
00:23:42,770 --> 00:23:41,220
don't know Mass specs is an acronym for

587
00:23:44,049 --> 00:23:42,780
the mass spectrometer for planetary

588
00:23:46,490 --> 00:23:44,059
expert well

589
00:23:47,750 --> 00:23:46,500
enter export yes Mass Spectrum for

590
00:23:49,730 --> 00:23:47,760
Planetary Exploration that's going to be

591
00:23:54,350 --> 00:23:49,740
going on Europa clipper

592
00:23:56,510 --> 00:23:54,360
um but that can do grains but those sort

593
00:23:59,529 --> 00:23:56,520
of instruments have issues with some of

594
00:24:02,510 --> 00:23:59,539
the more refractory Organics and some

595
00:24:04,669 --> 00:24:02,520
inorganic species and so what you really

596
00:24:07,070 --> 00:24:04,679
need to be able to do this given that

597
00:24:09,590 --> 00:24:07,080
you have enough cost margin is you need

598
00:24:10,970 --> 00:24:09,600
a dust detector or a grain like some

599
00:24:12,649 --> 00:24:10,980
sort of impact ionization Mass

600
00:24:15,110 --> 00:24:12,659
spectrometer that can utilize these

601
00:24:16,610 --> 00:24:15,120
hyper velocity impacts as an ionization

602
00:24:19,070 --> 00:24:16,620
source to determine ice grain

603
00:24:20,990 --> 00:24:19,080
composition and also something where you

604
00:24:22,730 --> 00:24:21,000
can assess the composition of the plume

605
00:24:33,770 --> 00:24:22,740
gas as well

606
00:24:33,780 --> 00:24:45,470
missions

607
00:24:51,649 --> 00:24:46,450
um

608
00:24:55,909 --> 00:24:53,630
a couple of slides

609
00:24:58,789 --> 00:24:55,919
um so it's in eccentric orbit the

610
00:25:00,950 --> 00:24:58,799
various intric orbit around Saturn and

611
00:25:02,510 --> 00:25:00,960
so if you look at I don't know can you

612
00:25:05,630 --> 00:25:02,520
see the the curse okay yeah you can

613
00:25:08,149 --> 00:25:05,640
right here see that little Green Dot

614
00:25:10,909 --> 00:25:08,159
um that's where the their every orbit

615
00:25:12,470 --> 00:25:10,919
you do like a small burn where you use a

616
00:25:14,990 --> 00:25:12,480
little bit of fuel to make sure that you

617
00:25:16,909 --> 00:25:15,000
stay uh in the orbit that you need to

618
00:25:18,710 --> 00:25:16,919
actually do these measurements and so

619
00:25:20,750 --> 00:25:18,720
it's not as huge of a deal and doesn't

620
00:25:23,870 --> 00:25:20,760
require like a ton of Delta V or like

621
00:25:25,430 --> 00:25:23,880
change in velocity of the spacecraft

622
00:25:26,870 --> 00:25:25,440
um but no that is something to consider

623
00:25:28,789 --> 00:25:26,880
and though you're you're right and that

624
00:25:30,769 --> 00:25:28,799
is something that we took into account

625
00:25:37,669 --> 00:25:30,779
when doing all these uh the orbital

626
00:25:42,710 --> 00:25:40,430
uh so the that's before we actually

627
00:25:45,110 --> 00:25:42,720
start science operations

628
00:25:47,630 --> 00:25:45,120
um because upon

629
00:25:50,029 --> 00:25:47,640
Saturn orbital insertion

630
00:25:53,090 --> 00:25:50,039
um we're going too fast

631
00:25:55,610 --> 00:25:53,100
um and the the spacecraft the

632
00:25:58,370 --> 00:25:55,620
inclination altitude geometry things

633
00:26:00,710 --> 00:25:58,380
like that aren't suitable to immediately

634
00:26:03,590 --> 00:26:00,720
enter science operations to start doing

635
00:26:06,169 --> 00:26:03,600
targeted Enceladus flybys and so we need

636
00:26:08,750 --> 00:26:06,179
to use Titan's gravity to further slow

637
00:26:10,250 --> 00:26:08,760
down so we can get within that goldilock

638
00:26:12,169 --> 00:26:10,260
zone that we talked about before for

639
00:26:20,910 --> 00:26:12,179
sampling

640
00:26:23,560 --> 00:26:21,250
[Music]