exploring ocean worlds - nasa · 6/9/2017 · exploring ocean worlds prebiotic and astrobiology...
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Exploring Ocean WorldsPrebiotic and Astrobiology Implications
Morgan L. Cable, Ph.D.
9 June 2017
Image: NASA/JPL-Caltech/SSI
Jet Propulsion LaboratoryCalifornia Institute of Technology
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What is an Ocean World?There are more than you think!
Images: Universal Pictures, NASA/JPL
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What is an Ocean World?There are more than you think!
Europa
Ganymede
Callisto
Images: NASA/JPL Note: Not to scale.
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4Images: NASA/JPL
Titan
Enceladus
Mimas
What is an Ocean World?There are more than you think!
Note: Not to scale.
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5Images: NASA/JPL Note: Not to scale.
Triton Pluto
What is an Ocean World?There are more than you think!
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6Images: NASA/JPL
What is an Ocean World?There are more than you think!
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Enceladus: Active, Astrobiologically Relevant, Accessible
Images: NASA/JPL
An ideal place to search for aqueous-based life
7
Ice crust
(2-10 km)
Global ocean
(18-22 km)
Hydrothermal
vents (>90°C)
South polar region with
active jets
Rocky (silicate)
core
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Enceladus: Active, Astrobiologically Relevant, AccessibleFree sample, no need to dig or drill
8Porco et al. (2014) Astron. J., 148, 3, 45.Images: NASA/JPL/SSI
• ~100 distinct, collimated jets emanating from Tiger Stripes that form a single plume
– Modulated by diurnal tidal flexing
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Enceladus: Active, Astrobiologically Relevant, AccessibleFree sample, no need to dig or drill
9Glein et al. (2015) Geochim. Cosmochim. Acta, 162, 202-219. Hsu et al. (2015) Nature 519, 207-210.Images: NASA/JPL
• ~100 distinct, collimated jets emanating from Tiger Stripes that form a single plume
– Modulated by diurnal tidal flexing
• Plume feeds the E ring
– Silica nanograins suggest recent hydrothermal activity
SiO2
2-9 nm
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Plume gas
– H2O, CO2, CH4, NH3, H2 (yay!), heavier hydrocarbons, simple and complex organics
– Mass flux: 200 kg/s
Plume CompositionOrganic-rich, sourced from the subsurface ocean
Waite et al. (2009) Nature 460, 487-490. Waite et al. (2017) Science 356, 155-159. Images: NASA/JPL/SwRI
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Plume grains
– Water-ice, salts (mostly NaCl), SiO2, high mass organic cations (HMOC)
– Mass flux: 50 kg/s (~10% of particles reach escape velocity)
Plume CompositionOrganic-rich, sourced from the subsurface ocean
Plume gas
– H2O, CO2, CH4, NH3, H2 (yay!), heavier hydrocarbons, simple and complex organics
– Mass flux: 200 kg/s
Postberg et al. (2009) Nature, 459, 1098-1101. Postberg et al. (2017) LPSC abstract no. 1401. Images: NASA/JPL/F. Postberg
H2O-ice species
Na clusters
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Images: NASA/JPL/Kelley/U. of Washington/IFE/URI-IAO/NOAA
May have been how life originated on Earth
12Kelley et al. (2005) Science, 307, 1428-1434.
Hydrothermal Vents?
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Enceladus Awaits
Images: NASA/JPL
An ideal place to search for aqueous-based life
13
Ice crust
(2-10 km)
Global ocean
(18-22 km)
Hydrothermal
vents (>90°C)
South polar region with
active jets
Rocky core
WE NEED TO GO BACK
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ENCELADUS LIFE FINDER
Jonathan I. Lunine (PI), Hunter Waite (DPI), Linda J. Spilker (PS), Morgan L. Cable (DPS)
and the ELF Science Team
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Europa Beckons
15Images: NASA/JPL
Jem of the Jovian system
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Europa Beckons
16Images: NASA/JPL Pre-Decisional – For Information and Discussion Purposes Only
Jem of the Jovian system
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17Video: NASA/JPL Europa Lander SDT Report. https://solarsystem.nasa.gov/docs/Europa_Lander_SDT_Report_2016.pdf
Europa BeckonsJem of the Jovian system
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Europa Beckons
18Images: NASA/JPL Pre-Decisional – For Information and Discussion Purposes Only
Jem of the Jovian system
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Europa Beckons
19Images: NASA/JPL Pre-Decisional – For Information and Discussion Purposes Only
A robust approach to search for signs of life
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Europa Beckons
20Figure: K. Hand
Keeping it all in context
1976
1953 1977
PCR Invented
1983
Hydrothermal vents discovered
DNA discovered
Viking Landers
2017
Human genome sequenced
2003
Tree of Life Then…
Europa Lander SDT Report delivered
2016
…Tree of Life Now.
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21Image: NASA-JPL
• Atmosphere– 96% N2, 4% CH4
– 1.5 bar (thicker than Earth)
• Surface– Water-ice coated in organics
– Dunes in the equatorial region
• Hydrologic Cycle– Liquid methane, ethane lakes
– Methane clouds, drizzle
• Putative Cryovolcanoes– Slurry of ammonia and water
ice, possibly methanolIR specular reflection off Jingpo Lacus captured by Cassini VIMS
(NASA/JPL/ Univ. of Arizona/DLR)
A possible cryovolcano in the Sotra Facula region of Titan(NASA/JPL/Univ. of Arizona/USGS)
Titan TantalizesFamiliar, yet alien
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Titan TantalizesFamiliar, yet alien
TITANClouds
EARTHClouds
22Images: NASA/JPL-Caltech/SSI; NASA
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Titan TantalizesFamiliar, yet alien
TITANRiver channels
EARTHRiver channels
23Images: NASA/JPL-Caltech; NASA/Landsat
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Titan TantalizesFamiliar, yet alien
TITANLakes and Seas
EARTHLakes and Seas
24Images: NASA/JPL-Caltech/ASI/Cornell; Google Earth
Surface area:
126,000 km2
Surface area:
58,000 km2
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Titan TantalizesFamiliar, yet alien
TITANRemnants of Ridges (Karst)
EARTHRemnants of Ridges (Karst)
10 km
Malaska et al., LPSC (2010), Abstract 1544
1 km
25Images: NASA/JPL-Caltech; Google Earth
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Titan TantalizesFamiliar, yet alien
TITANDune Fields
EARTHDune Fields
26Images: NASA/JPL-Caltech/ASI/Cornell; NASA/Landsat
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Titan Laboratory ExperimentsTackling Titan’s surface chemistry, one experiment at a time
Atmospheric
chemistry
products
Hydrocarbon
precipitation
Soluble
materials
dissolution
Fluvial
transport
subsurface transport?
Volatile
hydrocarbon
evaporation
Volatile
condensation
Lakes / evaporite playas
caves?
27Figure by M. Malaska
What happens when things evaporate from a Titan lake?
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Titan Laboratory Experiments: Surface DepositsProbing the bathtub rings around Titan’s lakes
Barnes J.W. et al., 2011, Icarus, 216, 136-140.
• Solubility of benzene in liquid ethane is low
• Benzene could be an abundant evaporite around the lakes on Titan
28
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Titan Laboratory ExperimentsTackling Titan’s surface chemistry, one experiment at a time
29Photo/images by M. Cable
LN2
C2H6 Heater
Steel spheres
Stir bar
Temperature probe~
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Titan Laboratory Experiments: Surface DepositsRecrystallization occurs when benzene and ethane are mixed
100 µm 100 µm
Before After 15 minutes
Cable, M. L. et al., 2014, Geophys. Res. Lett., 41, 5396–5401. 30Images: M. Cable, T. Vu
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Titan Laboratory Experiments: Surface DepositsRecrystallization occurs when benzene and ethane are mixed
Inte
nsity
3100305030002950290028502800
Raman shift (cm-1
)
With trapping No trapping Benzene control
AfterBefore
Benzene alone ethane benzene
31Vu, T. et al., 2014, J. Phys. Chem. A, 118, 4087–4094.
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Titan Laboratory Experiments: Surface DepositsWhat does it look like?
Benzene (C6H6) Ethane (C2H6)
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Titan Laboratory Experiments: Surface DepositsOur best guess . . .
Boese et al., 2003, Helv. Chim. Acta, 86, 1085-1100.
Proposed co-crystal configuration:
Acetylene/benzene co-crystal structure:
33
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Titan Laboratory Experiments: Surface DepositsX-rays, figuring out what stuff is made of since 1912
34Image: nothingnerdy.wikispaces.com
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Titan Laboratory Experiments: Surface Deposits
2:1 Benzene:EthaneRatio
Our best guess . . . was way off!
35Maynard-Casely et al., 2016, Int. Union of Crystallography J., 3,1-8.
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2:1 Benzene:EthaneRatio
36
Titan Laboratory Experiments: Surface DepositsOur best guess . . . was way off!
Maynard-Casely et al., 2016, Int. Union of Crystallography J., 3,1-8.
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Titan Laboratory Experiments: Surface DepositsTitan’s version of a hydrated mineral
37Image: M. Malaska
Is this co-crystal unique, or can other Titan molecules do the same thing?
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Titan Laboratory Experiments: Acetylene and AmmoniaAnother co-crystal?
38
Evidence of Cryovolcanism
Image: NASA/JPL Caltech/USGS/University of Arizona
10 km
• Acetylene is present on Titan– Detected in the atmosphere by INMS1
and on the surface by Huygens GC-MS2
• Ammonia may also exist on Titan’s surface today
– The origin of Titan’s nitrogen-rich atmosphere is most likely ammonia ice1,3
– Mixing could occur via cryovolcanism or other surface processes4
1) Waite, J. H. et al., 2005, Science, 308, 982-986.2) Niemann, H. B. et al., 2010, JGR, 115, E12006.3) Mandt, K. E. et al., 2014, Astrophys. J. Lett., 788, L24, 1-5.4) Lopes R. M. C. et al., 2013, JGR, 118, 416-435.
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Titan Laboratory Experiments: Acetylene and AmmoniaNew features in Raman
39
50 150 250 350 450 550 650 750
Inte
nsity
Raman Shift (cm-1)
Acetylene
Co-Crystal
Ammonia
197 cm-1
669 cm-1
722 cm-1
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Astrobiological ImplicationsRethinking our requirements for life
40Image: NASA-JPL/Caltech
Earth Titan Interaction/Bond Strength
Ionic Bond Covalent Bond Permanent or semi-permanent
Covalent BondHydrogen bonds,
π-bonds
Can be made/broken on timescales
relevant for life (ATP, proteins, etc.)
Hydrogen bonds,
π-bonds
van der Waals
forces
Loose associations that help hold
together secondary structures
At cryogenic temperatures, weaker forces become more important in molecular interactions
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Titan Laboratory Experiments: ConclusionsLearning what makes Titan tick
• Titan’s surface landscape is strongly influenced by a complex organic cycle.
• Molecules dissolve, precipitate and reorganizereadily, leading to novel solid geological materials.
• What’s needed?More lab work! Future missions!
41Image: ESA/ATG Medialab
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The makings of a truly Grand Finale
Cassini Mission to Saturn: Latest Discoveries
42Images: NASA-JPL/Caltech
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The makings of a truly Grand Finale
Cassini Mission to Saturn: Latest Discoveries
43Animation: NASA-JPL/Caltech/E. Sturm
Ring-Grazing orbitsGrand Finale orbitsImpact orbit
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The makings of a truly Grand Finale
Cassini Mission to Saturn: Latest Discoveries
44Image: NASA-JPL/Caltech
• Saturn internal structure
– Magnetic & gravity high-order moment measurements
• Ring mass
– Address age of main rings
• In-situ measurements
– Ionosphere, inner radiation belts, auroralregion, and D ring particles
• Ring mass
– Address age of main rings
• High resolution observations
– Rings, poles/aurora, atmosphere
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Pan in all its glory
Cassini Mission to Saturn: Latest Discoveries
45Images: NASA-JPL/Caltech
150 m/pixel (500 feet/pixel)
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Daphnis making waves
Cassini Mission to Saturn: Latest Discoveries
46Images: NASA-JPL/Caltech
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Plunging through the gap
Cassini Mission to Saturn: Latest Discoveries
47Animation: NASA-JPL/Caltech/E. Sturm
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Plunging through the gap
Cassini Mission to Saturn: Latest Discoveries
48Animation: NASA-JPL/Caltech/SSI
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AcknowledgementsSo long, and thanks for all the fish
• Rob Hodyss
• Tuan Vu
• Mike Malaska
• Mathieu Choukroun
• Helen Maynard-Casely
• Patricia Beauchamp
• NASA Astrobiology Institute
• NASA Solar System Workings Program
• Australian Nuclear Science and Technology Organization (ANSTO)
Jet Propulsion LaboratoryCalifornia Institute of Technology
• Kevin Hand, Study Co-Lead
• Alison Murray, Study Co-Lead
• James Garvin, Study Co-Lead
• Cynthia Phillips
• Amy Hofmann
• The Europa Lander Science Definition Team
• The entire Europa Lander Team
• Earl Maize, Project Manager
• Linda Spilker, Project Scientist
• Trina Ray, Science Sys Eng
• Erick Sturm, Mission Planning
• The entire Cassini Team
Titan Lab Work Europa Lander Cassini Mission
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ENCELADUS LIFE FINDER
Morgan L. Cable, Jonathan I. Lunine, Linda J. Spilker and the ELF Science Team
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ELF as the Next Logical Step
Images: NASA/JPL/SwRI/F. Postberg
A robust instrument suite that targets plume gas and grains to search for life
52
MASPEXMass Spectrometer for Planetary Exploration
ENIJAEnceladus Icy Jet Analyzer
• Target: Plume gas• Extended mass range for heavy organic molecules• Enhanced mass resolution for critical isotopes• Enhanced dynamic range for high S/N• Improved sensitivity (better than 1 ppt with
cryotrap) for rare noble gases
• Target: Plume grains• Heritage: Giotto, Stardust CIDA but improved ion
optics, ion detector, spectra processing• Segmented target for low and high-rate spectra
mode (compositional profile with 100 m spatial resolution)
• Complete composition of each ice grain, over a wide mass range
Pre-Decisional – For Information and Discussion Purposes Only
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Plume Modeling
Images: B. Teolis/B. Southworth
Know before you go
53
Plume Gas Model Plume Grain Model
Pre-Decisional – For Information and Discussion Purposes Only
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ELF Mission Ops
Images: NASA/JPL
Life detection on the fly
54Pre-Decisional – For Information and Discussion Purposes Only
• 10 flybys, each at 5 km/s
• 62-day orbit allows ample time to set instrument parameters for the next flyby
Ambient
Science Mode
Comm
OTM
DeSat
Solar Array
Slew
Comm
OTM
(inc. Warm-Up)
S/c slew to
flyby attitude
Quicklook comm
Solar Array
and s/c slew to flyby attitude
OTM
Comm
Cryo Science
Mode
Cryo Science
Mode
Cryo Science
Mode
~1500 Whr
Recharge (10 days)
~500 Whr
Recharge (3 days)
Only period
where arrays are
not pointed
at Sun (5 hours)
DeSat
Battery Recharge Mode
Science Mode
Slewing Mode
Prop Mode
Comm Mode
(OTM = Orbit Trim Maneuver)
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ELF Science Investigation
Images: NASA/JPL/SwRI
Three objectives, one profound question: Is there life beyond Earth?
55
Reactions with Water Hydrothermal AlterationNitrogen as an Indicator
1a. Determine the original molecular carrier for nitrogen as an indicator of the degree of volatile evolution on Enceladus.
1b. Quantify the fraction of the volatile population that has not reacted with liquid water.
Science Objective 1: EvolutionDetermine if Enceladus’ volatiles, including organics, have evolved over time.
1c. Confirm if the ocean has been, or is, in contact with hydrothermal systems at its base.
Pre-Decisional – For Information and Discussion Purposes Only
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ELF Science Investigation
Images: NASA/JPL
Three objectives, one profound question: Is there life beyond Earth?
56
Redox Energy pHTemperature
2a. Determine the temperature of the ocean and possible hydrothermal systems to within 100 K.
2b. Quantify the amount of redox energy available.
2d. Determine the pH of the ocean to within an accuracy of 1 unit.
Science Objective 2: HabitabilityDetermine if the ocean of Enceladus satisfies the basic requirements of habitability.
Oxidation State
2c. Determine the oxidation state of the ocean.
Pre-Decisional – For Information and Discussion Purposes Only
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ELF Science Investigation
Images: NASA/JPL
Three objectives, one profound question: Is there life beyond Earth?
57
Membrane Molecules Isotopic TrendsAmino Acids
3a. Look for patterns in the amino acid distribution indicative of biological synthesis, e.g. underrepresentation of glycine relative to other amino acids that are energetically more difficult to form.
3b. Determine the long-chain fatty acid (C12–C30) distribution to look for patterns such as the even-odd disparity due to C2 addition in biological synthesis.
3c. Determine the hydrocarbon abundance distribution, D/H ratio and the 13C/12C distribution in hydrocarbons and CO2, to look for patterns consistent with biological synthesis.
Science Objective 3: LifeDetermine if the plume of Enceladus contains chemical signatures of biology.
Pre-Decisional – For Information and Discussion Purposes Only
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A Life Investigation Within Reach
Images: NASA/JPL
Multiple, independent tests for life shrink the ambiguity box
58Pre-Decisional – For Information and Discussion Purposes Only
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Enceladus Awaits
Images: NASA/JPL
An ideal place to search for aqueous-based life
59
• There is definitive evidence of a subsurface ocean with organics, salts, and free energy.
• The plume of Enceladus includes ocean material and is readily analyzed for evidence of life—a goal of the Enceladus Life Finder.
Pre-Decisional – For Information and Discussion Purposes Only