Mission to Europa. Brian Kristall, Matthew Strumpf, Josh Townsend, Oliver Williams
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1 Mission to Europa Brian Kristall, Matthew Strumpf, Josh Townsend, Oliver Williams
2 The Family Portrait: Galilean Satellites NASA/JPL Io Europa Ganymede Callisto Moon Radius (km) Mass (10 21 kg) Mean density (g cm -3 ) Surface Temperature (K) Period (days) Eccentricity Semimajor axis (RJ) Chyba & Phillips, 2007
3 Interior Models of Europa: Gravity Field Indicates Complete Differentiation NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
4 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
5 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
6 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
7 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick Ocean vs. Ice - Magnetometer NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
8 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick Ocean vs. Ice - Magnetometer Europan induced magnetic field NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
9 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick Ocean vs. Ice - Magnetometer Europan induced magnetic field Varies in direction + strength to Jupiter s magnetic field NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
10 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick Ocean vs. Ice - Magnetometer Europan induced magnetic field Varies in direction + strength to Jupiter s magnetic field Requires near-surface, global, electrically conducting layer NASA/JPL Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
11 Interior Models of Europa: Gravity Field Indicates Complete Differentiation Central Core Fe/Fe-S Anhydrous Rocky Mantle Surface Layer ρ 1 g cm -3 ~100 km thick NASA/JPL Ocean vs. Ice - Magnetometer Europan induced magnetic field Varies in direction + strength to Jupiter s magnetic field Requires near-surface, global, electrically conducting layer Requires nearly complete spherical shell Anderson et. al., 1998 Kivelson et. al., 2000 Zimmer et. al., 2000
12 Tidal Heating & Volcanism on Galilean Satellites NASA/JPL Flexing of tidal bulge produce internal dissipation of energy Tidal bulge height varies with distance from Jupiter eccentricity = variability NASA/JPL
13 Tidal Heating & Volcanism on Galilean Satellites NASA/JPL Flexing of tidal bulge produce internal dissipation of energy Tidal bulge height varies with distance from Jupiter eccentricity = variability Europa ~1.6X further, ~2.5X eccentricity of Io NASA/JPL
14 Tidal Heating & Europan Seafloor Volcanism and Hydrothermal Systems? Thin Ice Shell Thick Ice Shell NASA/ESA Modeled Heat Flow mw m -2 (McKinnon & Shock, 2001)
15 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer NASA/JPL McCord et. al., 1999; Carlson et. al., 1999
16 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer Water Ice NASA/JPL McCord et. al., 1999; Carlson et. al., 1999
17 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer Water Ice Hydrated Salts? Mg-SO4-hydrates Na-Mg-SO4-hydrates Na-CO3-hydrates Na-SO4-hydrates NASA/JPL McCord et. al., 1999; Carlson et. al., 1999
18 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer Water Ice Hydrated Salts? Mg-SO4-hydrates Na-Mg-SO4-hydrates Na-CO3-hydrates Na-SO4-hydrates Hydrated Sulfuric Acid? NIMS end-members NIMS-hydrate H2SO4 8H2O H2SO4 nh2o NASA/JPL McCord et. al., 1999; Carlson et. al., 1999
19 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer Water Ice Hydrated Salts? Mg-SO4-hydrates Na-Mg-SO4-hydrates Na-CO3-hydrates Na-SO4-hydrates Hydrated Sulfuric Acid? Minor SO2, H2O2, CO2 H2SO4 nh2o NIMS end-members NIMS-hydrate H2SO4 8H2O NASA/JPL McCord et. al., 1999; Carlson et. al., 1999
20 Europan Surface Composition: Galileo s Near-Infrared Mapping Spectrometer Water Ice Hydrated Salts? Mg-SO4-hydrates Na-Mg-SO4-hydrates Na-CO3-hydrates Na-SO4-hydrates Hydrated Sulfuric Acid? Minor SO2, H2O2, CO2 BLUE = more salts YELLOW-ORANGE = more ice NASA/JPL-Caltech
21 Europan Surface Geology Limited impact craters indicate young surface age Tyre Impact Scar ~140 km wide Pwyll Crater ~26 km wide NASA/JPL/ASU
22 Europan Surface Geology Ridge Plains & Double ridges km wide, m tall, km long Image 20 x 20 km Ridge ~2.6 km wide ~300 m high Image 14 x 17 km NASA/JPL Greeley et. al., 2000
23 Europan Surface Geology Ridge Plains & Double ridges km wide, m tall, km long NASA/JPL/DLR
24 Europan Surface Geology Bands - multiple parallel lines little topographic expression Astypaleae Linea fault >800 km long Image 24 x 16 km NASA/JPL/ASU
25 Europan Surface Geology Chaotic Terrains - Rafted iceberg-like blocks Conamara Chaos Image 70 x 30 km NASA/JPL/ASU
26 Yeah, right! Europa Technical Challenges 1. Drilling through km s (?) of ice 2. Jovian radiation 3. Others Picture: NASA JPL
27 Drill Baby Drill! Using existing technology, a small (10 inch diameter) heated-drill could drill an estimated 10 cm/day. Even most hopeful estimates put thickness of ice crust at 10km. Time required to drill 10km = days. Not very feasible!
28 Drilling Dillema Solution: Don t drill (all the way) Small drill arm could drill several cm s Pristine samples of Europan ice
29 Jovian Radiation: Overview Jupiter magnetic field 20,000x Earth magnetic field. Radiation source from charged particles in Jupiters mag. field. Europa orbit annual radiation dose 3 million x human annual dose. Europan surface dose halved.
30 Jovian Radiation: Effects Damage to electronics from electrostatic discharge. Parasitic currents. Spurious noise introduced to detectors/ sensors. Source: NASA-ESA Outer Planet Mission Study
31 Jovian Radiation: Mitigation Orbit 2.9Mrad in orbit around Europa. Protect orbiter/lander with Al-shielding and radhardened parts. Minimize radiation exposure by special positioning of orbit. Surface Surface landing: Radiation halved. Source: Above: Shielded circuitry part of the ESA Planck satellite. Source: NASA-ESA Outer Planet Mission Study
32 Other Challenges Europan orbiter/lander must regulate temperature. Landing on body with no atmosphere, can t parachute! Periodic communication blackouts due to orbit. Sterilizing orbiter/lander. Russian Space Agency Europa Lander concept. Source:
33 Ethical Issues Nuclear power source Contamination of Europa Leaving equipment on surface and in ocean Introducing non-native life from Earth
34 Nuclear Power Weight efficient Hazard to human health Accident in construction Failure in launch Nuclear waste from enrichment Convince the public
35 Why prevent contamination? Terrestrial life taints currently pristine Europa "false positives" Safe guard future scientific exploration of Europa and its biological potential Protect possible native Europan life Required under UN Treaty on Principles Governing the Activities of States in the Exploration and Use of Outer Space, Including the Moon and Other Celestial Bodies
36 Task Group on the Forward Contamination of Europa Commission on Physical Sciences, Mathematics, and Applications (Space Studies Board) Produced "Preventing the Forward Contamination of Europa" in 2000 David Stahl, Northwestern University
37 Task Group Findings NASA requirements for contamination prevention efforts based on likelihood of body harboring life Current requirements are satisfactory Isopropyl alcohol, hydrogen peroxide, dry heating, clean room assembly, bioload tests, final sterilization by Jupiter's radiation Recommended studies to define issues Clean room practices, bioload assay methods, radiation resistant microbes, autotroph detection
38 Task Group Disagreement Majority: bioload reduced so that probability of contaminating viable terrestrial organism is 10e-4 Minority: less stringent requirements (Vikinglevel cleaning) No reason for enhanced policies Radiation will kill, life will not survive and multiply in Europan ocean
39 Mission Objectives Characteristics of ice and salts Characteristics of sub-surface ocean Internal structure Life?
40 Ice Chemical Composition Surface water Chemistry Is life even possible? Physical characteristics Thickness Mid-ocean ridge?
41 Ocean Chemical Composition Depth Relation to the interior Ice-ocean exchange and relationship
42 Formation of surface processes Smokers Hydrothermal vents Physical Characteristics Try to find a site for future exploration Possible thin spot for drilling
43 Radiation, Gravity, Magnetism Effects of extreme radiation due to Jupiter Tidal bulges from gravitational pull Presence of a magnetic field
44 Life Is life even possible on Europa? Are there hydrothermal vents? If not, is life likely to be found? Should we continue the search in the ocean? Should we find a thin section of ice and drill? Would we even recognize if we found life?
45 Equipment Orbiter Map Europa s surface Characterize ocean Relay information Orbiter instruments: Magnetometer Laser altimeter Radio Science Ice Penetrating Radar VIS-IR Imaging Spectrometer UV Spectrometer Ion and Neutral Mass Spectrometer Thermal Instrument Narrow Angle Camera Wide Angle Camera and Medium Angle Camera Magnetometer Particle and Plasma Instrument Nasa/JPL
46 Equipment Surface lander Sample the ice (drill a few centimeters) Deploy seismometer Ocean depth Ice thickness
47 Budget & Time Line JEO Phase A-F lifecycle NASA: $4 billion JGO Phase A-F lifecycle ESA: 650 million
48
49
50 The Family Portrait: Galilean Satellites
51
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