NEO Sample Return Mission

Transcription

1 Cannes, 5 Juin 2008 M.A. Barucci & M. Yoshikawa MARCO POLO NEO Sample Return Mission This mission, prepared by a joint European Japanese team, is supported by more than 450 confirmed scientists.

2 Joint Assessment Study (ESA-JAXA) ESA Science Team: M.A. Barucci (LESIA, Paris Observatory, F), M. Yoshikawa (JSPEC/JAXA, J), D. Koschny (ESTEC/ESA, NL), H. Boehnhardt (MPI, Lindau, D), J.R. Brucato (INAF-OAC, Naples, I), M. Coradini (ESA, Paris, F), E. Dotto (INAF-OAR, Rome, I), I.A. Franchi (Open University, UK), S.F. Green (Open University, UK), F), J.-L. Josset (SPACE-X, CH), P. Michel (OCA, Nice, F), J. Kawagushi (JSPEC/JAXA, J), K. Muinonen (Univ. Helsinki Observatory, FI), J. Oberst (DLR, Berlin, D), H. Yano (JSPEC/JAXA, J) and R. Binzel (MIT, USA)

3 A NEO-SR mission is in the priority of CV 1. What are the conditions for Planet formation and the emergence of Life? 2. How does the Solar System work?

4 In the early solar nebula, the dust accreted to form planetesimals and the planetesimals accreted to form planetary embryos. In the asteroid belt this process was stopped when Jupiter formed. CAIs?? D C Chondrules Eucrites Differentiation HED differentiation Planetesimal Differentiation Planetary Accretion Mesosiderites Earth Mars Angrites Pallasites

5 Asteroids and Comets in the Inner Solar System NEO IEO SOURCE

6 Origin of the Life: The planets of the inner Solar System experienced an intense influx of (organic-rich) cometary and asteroidal material for several hundred million years after they formed. The earliest evidence for life on Earth coincides with the decline of this enhanced bombardment. The complex organics in this influx appears to contain a left-handedness - offering a tantalising possibility that they may be related to the origin of life.

7 Main questions: 1) What were the initial conditions and evolution history of the solar nebula? 2) Which were the properties of the building blocks of the terrestrial planets? 3) How did major events (e.g. agglomeration, heating,.. ) influenced the history of planetesimals? 4) Do primitive classe objects contain presolar material yet unknown in meteoritic samples? 5) What are the organics in primitive materials? 6) How NEO organics can shed light on the origin of molecules necessary for life? 7) What is the role of NEO impacts in the origin and evolution of life on Earth?

8 The accessibility of NEOs NEA ACCESSIBILITY H-PLOT Sample Update 02/2007: 3238 objects with H<22 PHAETHON EPHAISTOS P/ENCKE delta-v (km/sec) Mercury EROS 2001SG FG3 2002AT4 OLJATO Asteroid Main Belt Jupiter WILSON-HARRINGTON 4 2 Venus 1993JU3 Mars ITOKAWA NEA population (H<22) short-period comets dormant comets NEAs visited SR mission targets 0 EARTH aphelion distance (AU)

9 Baseline Marco Polo to 4015 Wilson-Harrington (C type) Launcher : Soyuz Fregat (indirect injection):

10 Other possible scenarios, all involving Soyuz Fregat

11 Target: 1989 UQ (C type) Launch, 22/09/2017 Earth swing by, 20/09/2018 Venus swing by, 05/03/2019 Arrival, 20/12/2020 Science operations 1.62 years Departure, 18/07/2022 Venus swing by, 25/06/2023 Earth arrival, 19/11/2023 Total mission duration: 6.2 years

12 MARCO POLO Proposal Mission scenario mapping cruise phase spacecraft ERC sampling system landing and sampling propulsion module Lander NEO science phase remote sensing package Launch in situ analyses TTC relay re-entry phase Earth return phase Operations

13 Scientific objectives of MARCO POLO What were the initial conditions and evolution history of the solar nebula? Do primitive classe objects contain presolar material yet unknown in meteoritic samples? Which were the properties of the building blocks of terrestrial planets? Composition of primitive material What was the role of NEO impacts in the origin of life? How did composition vary with geological context? How did space weathering and collisions affect NEO composition? Interior Elemental/Isotopical composition Nature of organics Mineralogy Surface morphology Mass, gravity density Internal structure Sample collection & return Orbiter Lander

14 Hi-Res Camera Radio Science V-NIR Spectrometer MIR Spectrometer γ-rays Spectrometer X-rays Spectrometer & Solar Monitor SCIENCE Dust Environment Orbital & Rotational Evolution Morphology, Topography Macroscale Dust & Regolith Size,Shape,Mass,Gravity,Density Internal Structure, Stratigraphy Macroscale Mineralogy Macroscale Elemental composition Space weathering Detailed stratigraphy Microscale analyses Dust Monitor Laser Altimeter Radar Neutron Counter Neutral Particle Detector LANDER

15 MARCO POLO is a flexible mission with several possible options and several possible high interest targets. The various phases of the mission are scientifically autonomous. The completion of each of them separately will lead to a major improvement of our knowledge. Highest priority : Returned Samples of inestimable scientific value - most primitive organic materials - earliest fundamental planetary building blocks Minimum achievement : first remote sensing data from a primitive body Additional opportunity : In situ data, if a Lander (Philae heritage) is added, will also represent a premier in asteroid science.

16 MARCO POLO SPACECRAFT Marco Polo Spacecraft Hayabusa Spacecraft 5.0 m 2.2 m 4.2 m 1.8 m 1.0 m 1.4 m 1.4 m 4.0 m 1.1 m >1.5 m 1.0 m Minerva hopper Lander: Philae heritage >5.0 m 50m Obstacles of equivalent-size as the spacecraft are what MP must avoid as a long arm for sampling as the size of solar arrays is needed 10m

17 Extendible Boom Candidates Several options (e. g. from DLR, ISAS, Spain) exist for the extendible boom to be deployed and retracted for the touch-and-go sampling with high TRL including the space-flown heritages. Verification tests and modification for asteroid sampling are now in progress. System Coilable Mast High-Rigidity Mast Bi-STEM SPINAR Robotic Arm Axial Strength Strong Strong Moderate Weak Strong (Depending on design) 5m Extension and Retraction Capable Capable Capable Capable in principle Capable Weight Light Heavy Moderate Ligh Heavy Stored Volume Small Large Small Small Large Space-flown Heritages SFU-SAP (ISAS) Geotail, (ISAS) AKEBONO (ISAS) SFU-2D/HV (ISAS) HALCA (ISAS) HST Voyager Mars Path Finder ISAS Sounding Rocket CANADARM (CSA) MER (NASA)

18 Corer Projectile Development Experimental Set-Up Allows the collection of samples with stratigraphic integrity Porous Asteroid/ Comet Analogs Dual Corer Concept sand pumice Hayabusa Sampling Horn Pumice board

19 Sticky Pad (tested in micro-gravity environment) Capacity: 10g up /1s to 100 g Grain size: µm cm Increasing the applied force increases the contact with the simulant and thus increases the yield of each sample. A: 67N; B:111N; C:160N; D:200N Johns Hopkins University Applied Physics Laboratory

20 Sample acquisition and transfer system ERC EA SC Car SH BC LM Sampling and transfer mechanisms and units: Rotary Corer (RC) with shutter: Corer = Sample Vessel (3 x) Extendable Arm (EA) for sampling SH & Back Cover (BC) on Carousel (Car): Lift mechanism (LM) supports SH and back cover on Carousel: Back Cover Sample Container- Lock RC CDF Marco Polo Study

21 Laboratory investigation: High spatial resolution and analytical precision are needed: High precision analyses - including trace element abundances to ppb levels and isotopic ratios approaching ppm levels of precision High spatial resolution - a few microns or less Requires very specific sample selection and preparation. Requires large, complex instruments e.g. high mass resolution instruments (large magnets, high voltage), bright sources (e.g. Synchrotron) and usually requires multi-approach studies

22 Mineralogical, Chemical and Isotopic Characterization of Primitive Materials Identify Early Solar System Chronology Search for Unique Pre-solar Grains Astrobiological Significance

23 Conclusion: MARCO POLO has the potential to revolutionize our understanding of primitive materials essential to understand the conditions for planet formation and emergence of life. It can provide us important information needed to develop strategies to protect the Earth from the potential hazards represented by NEO collisions. Moreover sample return mission to NEOs will be pathfinder for sample returns from high gravity bodies and, later on, for human missions that might use asteroid resources to facilitate human exploration and the development of space. Current Status for the Mission Oct. 2007: Selected by ESA on COSMIC VISION program for a joint assessment study (JAXA-ESA) April 14: Final ESA CDF study May 2008: ESA ITT for a phase A Industrial Study June 2008: Declaration of Interest in Science Instrumentation Sept. 2009: Selection for Definition Phase