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In-situ instrumentation for planetary surface exploration: present and future

In-situ instrumentation for planetary surface exploration: present and future. M. Hilchenbach. Lindau, June 27, 2003. In-situ instrumentation instrumentation on the surfaces of planets, asteroids, moons or comets - goals: measurement of elemental and isotopic composition,

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In-situ instrumentation for planetary surface exploration: present and future

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  1. In-situ instrumentation for planetary surface exploration: present and future M. Hilchenbach Lindau, June 27, 2003

  2. In-situ instrumentation instrumentation on the surfaces of planets, asteroids, moons or comets - goals: measurement of elemental and isotopic composition, mineralogy and soil parameters, geological history, search for organic compounds on extraterrestrial bodies - methods: physical methods and applicable instrument designs: present and future

  3. Reaching planetary surfaces: example Mars: Entry, descent and landing

  4. Heavy elements and iron containing minerals Tools: APXS - Alpha, Protons and X-ray Sensor Mössbauer spectrometer (part of the payload of Nasa`s Martian rover missions Spirit and Opportunity, ESA`s Mars Express lander, Beagle II, ESA’s Rosetta mission)

  5. APXS - Alpha, Protons and X-ray Sensor I alpha backscattering detector

  6. APXS - Alpha, Protons and X-ray Sensor II X-Ray fluorescence detector

  7. APXS III - Observations Mars Pathfinder

  8. Martian and terrestrial sample compositions Rieder et al. 1997 Only the top layer composition is measured

  9. Mössbauer spectrometer I

  10. Mössbauer spectrometer II Determination of the oxidation state of minerals containing iron

  11. Sample Acquisition Systems in Space Applications

  12. Lunar Soil - Apollo 15

  13. Apollo Missions Handtools Gas Analysis Sample Container Tongs (Apollo 12) Scale Hammer Scoop Rake (Apollo 16) Gnomon (Apollo 15)

  14. Remote Sample Return Missions 30 years ago Luna 16, 1970 Drill Sealed Capsule On-orbit dry mass: 5600 kg Launch Date: 1970-09-12 Lunar soil in container: 0.1 kg Re-entry date: 1970-24-09

  15. Luna 24, 1976 Lunokhod 3

  16. Example: “Hard” material: Fractures in individual grains about 1 mm

  17. Sample Acquisition: Mini and Micro Gripper Microgrippers created in microstructurable glass: Operated by piezo - actor Nanotube Nanotweezers: Just voltage operated P. Kim and C. M. Lieber SCIENCE 286, p.2148, 1999 R. Salim et al. Microsystem Technologies 4, p.32, 1997

  18. Elements and isotopes - classification - objective: elemental and isotopic composition Tools: mass spectrometer

  19. Goldschmidt's Classification Lithophile: concentration in silicate materials, examples Na, Mg, Al, K or Ca Siderophile: elements that tend to concentrate in metallic iron, such as Mn or Ni Chalcophile: elements that concentrate in sulfide phases, examples Cu, Se or Pb Atmophile: volatile elements in atmospheres, such as H, He or Ar

  20. Objective Geochemistry of crust and regolith (rocks ?) Tool: Composition Measurement Bulk composition of the refractory, lithophile (Al, Ca, Mg, Ti, Be, Sc, V, Sr, Y, Zr, Nb, Ba, REE, Hf, Ta, Th, U), volatile lithophile (K, Na, Rb, Cl, F), refractory siderophile (Fe, Ni, Co, Mo, W), moderately to volatile siderophile or chalcophile (Ga, Ge, Au, Ag and S, Se, Cd, Hg), and atmophile elements (H, He, Ne, Ar, Kr, Xe). The most abundant elements (99%) are: O, Mg, Al, Si, Ca, Fe, K, Na Other element are ‘Trace Elements’. example: ‘Bulk Silicate Earth’

  21. Example of Lunar Soil Composition: i.e. trace elements such as Scandium and Samarium Wentworth 1994

  22. Trace elements as indicators Partitioning analysis via trace elements analysis Korotev 1997

  23. Surface history Surface erosion and “gardening” of surface by impacts ? Regolith Layer Impact History (‘Gardening’) Method: Identification of meteorite and cometary material or solar particles

  24. Measurement of the isotopic ratios

  25. History - Geochronology Radiogenic Isotopes Geochemistry Examples: 40K - 40Ar, 87Rb - 87Sr, 147Sm - 143Nd or 182Hf -182W (extinct nuclide chronometer) Presumably not achievable in-situ (lander)…. - required sensitivity - isobaric interferences

  26. Mass spectrometer instrumentation

  27. Example: “In situ” mass spectrometry W. B. Brinckerhoff, APL G. G. Managadze, IKI 2000 Laser desorption source and refectron type time-of-flight. Mass ~2 kg, Volume ~20x15x10 cm3 Mn/Fe ratio versus shot number Basalt: Mass spectrum Fe, Cr isotopes

  28. E B Energy-Mass Spectrograph for Measurement of Ions and Neutral Atoms Funsten 1996

  29. Hadamard transform time-of-flight mass spectrometer High duty cycle: about 50% Brock 1999

  30. Mass spectroscopy using a rotating electric field E time-of-flight phase Clemmons 1998

  31. Technology: Surface microstructure/miniature mass spectrometer Siebert, 1998 Manufacturing by lithographic 3D techniques (e.g. LIGA)

  32. Electrostatic Axially Harmonic Orbital Trapping: A High-Performance Technique of Mass Analysis A. Makarov 2000 Modes of operation: a) Fourier transform b) mass selective instability Mass spectrum in frequency domain

  33. A Capacitance Standard Based on Counting Electrons ‘Quantum dots’ Temperature 40 mK Keller 1999

  34. Mineralogy Tools - (infrared spectrometer) - Raman spectrometer

  35. Illustration (Moon) scale: 80 mm “Close-up” Lunar soil, Apollo 12 Landscape, Apollo 15 scale: 2.5 mm scale: 1 mm Photomicrograph of lunar basalt, Apollo 16 Orange volcanic glass (lava) and ilmenite (FeTiO3), Apollo 17

  36. Geochemistry: Minerals in the lunar regolith

  37. “In-situ” Mineralogy: Structure (and Composition) …. Oxides Sulphides Feldspars Silicates Meteoritic Minerals …. Example Olivine - Series between two end-members: Forsterite (Mg2SiO4) and Fayalite (Fe2SiO4), Olivine - Temperature, phase and molecular fractionation Example: Lunar regolith (Apollo 17 “Sample Return”) Position of 820 cm-1 peak shifts with Mg/Fe ratio Raman Spectrometry, Korotev 1997

  38. Organic compounds Goals identification and quantification of - traces of organic compounds in the Martian deep soil - organic compounds in the surface matter of a comet Tool - gas chromatograph coupled with a mass spectrometer

  39. Viking 1976 Result: no life detected, could not even identify organic molecules (< ppb) in the upper layer of the Martian soil.

  40. Science goal: Signs of Past and Present Life Are there any organic or water molecules in the Martian soil or atmosphere ? Detection and determination of organic compounds and water in Martian soil from different depths - Observation of oxidised organic compounds, not just CO2 ; Question: What are the oxidising agents ? Are they present in the deeper Martian soil layers ? - Identification and characterisation of minute traces of complex organic molecules, which might be contained and/or encapsulated in the subsurface material and are most likely very rare. Amino acid chirality determination. - Determination of elements essential for (terrestrial) life, such as C, O, N and H - Measurement of the isotopic ratios, such as D/H, 13C /12C, 15N/14N etc. - Traces of extinct life forms, even more interesting, traces of extant life forms

  41. Goal: identification and quantification of traces of organic compounds

  42. GC-MS: Gas chromatograph coupled to mass spectrometer Mass spectrometer Gas Tank injector column (detector) sample Schematic view

  43. Identification and characterisation of minute traces of complex organic molecules hydrolyzed HPLC analyis Glavin 1999 unhydrolyzed Benner 2000 Sample preparation and sample concentration is required prior to the GC-MS analysis. A GC-MS can only analyze volatile compounds. Most metastable products of organics substances are refractory (e.g. salts). The sample preparation (e.g. esterification) is an essential condition for the GC-MS analysis.

  44. Chemical derivatization

  45. Pyrolysis cell

  46. Cassini`-Huygens visit to the atmosphere of Saturn`s moon Titan

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