Lutetia/ESA Bernard Marty CRPG Univ. Lorraine F NASA Patrick Michel Univ. Nice CNRS OCA F On behalf of the MarcoPolo-R Science Team M. Champenois ESA CV M3 , 21 JAN. 2014 Science Study Team Lutetia/ESA M.A. Barucci (lead) P. Michel (co-lead) J.R. Brucato E. Dotto P. Ehrenfreund I.A. Franchi S.F. Green L.-M. Lara B. Marty Instrument PIs T. Andert (RSE, D) M.A. Barucci (MaRIS, F) NASA G. Cremonese (MaNAC, I) O. Groussin (THERMAP, F) J.-L. Josset (CUC, CH) E. Palomba (VISTA2, I) ESA D. Koschny (Study Scientist) D. Agnolon (Study Manager) J. Romstedt (Payload Manager) P. Martin, R. Chalex M. Champenois ESA CV M3 , 21 JAN. 2014 Cosmic Vision 2015‐2025 MarcoPolo-R addresses the scientific questions: 1) What are the conditions for life and planetary formation? 2) How does the Solar System work? Related issue with a Near-Earth Asteroid characterization: Impact hazard and mitigation ESA CV M3 , 21 JAN. 2014 Lutetia/ESA MarcoPolo-R will: • Return ~100g of sample for high NASA precision lab analysis • Characterize a primitive Near-Earth Asteroid at multiple scales M. Champenois ESA CV M3 , 21 JAN. 2014 Formaon & Evolu2on of the Solar System Hubble Space Telescope Orion Treasury Project Team Beta Pictoris, European Southern Observatory ESA CV M3 , 21 JAN. 2014 /orm12on 3 Evolu2on of the Solar System Proto Sun Protoplanetary DisC Dust + Gas Planetesimals However Planet /orm12on and Migr12on The Solar System today ESA CV M3, 21 JAN. 2014 Courtesy : S. Tachibana /orm12on 3 Evolu2on of the Solar System Proto Sun Protoplanetary DisC Small primi72e bodies6. Dust + Gas record compleI chemical and physical processes Planetesimals in the early Solar System However Large evolved bodies: Planet /orm12on and Migr12on . mel2ng 3 diHeren212on The Solar System today ESA CV M3 , 21 JAN. 2014 Courtesy : S. Tachibana Why sample return? Environmental control Adaptability Spatial M. Champenois P. Burnard resolution ESRF synchrotron faclility Stadermann et al., 2010 High energy Precision ESA CV M3 , 21 JAN. 2014 M. Champenois Sample return legacy Apollo NASA Luna Soviet Union Genesis Origin of the Moon NASA Accretion of planets Isotopic composition of the Sun N A S Stardust NASA A! Comet composition Large scale mixing Credits : NASA & JAXA Hayabusa JAXA first sample returned from (evolved S-type) asteroid ESA CV M3, 21 JAN. 2014 European cosmochemistry European teams at the forefront of sample return analysis • Cosmochemistry : a science born in Europe • Genesis: 2 of 4 scientific goals done by European labs • Stardust: 1/3 labs were European in the Preliminary Examination Team Ensisheim meteorite fall,Shedel, 1493 Analytical instruments used worldwide for ET samples designed and made in Europe • Cameca (F): ion probes • Nu Instruments (GB): mass spec. • Thermofisher (D): mass spec. ESA CV M3, 21 JAN. 2014 The next two decades : exploration of asteroids はやぶさ2ステッカー（w100×h87） HAYABUSA2 1999JU3 N A Hayabusa2 OSIRIS-REx S MarcoPolo-R JAXA NASA A! ESA • MarcoPolo.R will sample an uneIplored region of the disC • Prepare for human eIAlor12on of the Solar System Returning this sample will Ceep Europe at the forefront of planetary science ESA CV M3 , 21 JAN. 2014 The next two decades : exploration of asteroids はやぶさ2ステッカー（w100×h87） HAYABUSA2 1999JU3 N A Hayabusa2 OSIRIS-REx S MarcoPolo-R JAXA NASA A! ESA NASA committed to provide substantial contributions 1+1+1 >> 3 ! JAXA expressed interest Returning this sample will Ceep Europe at the forefront of planetary science ESA CV M3 , 21 JAN. 2014 Grand questions on the origin and evolution of the Solar System 1. What was the astrophysical setting of the birth of the Solar System ? 2. What is the origin and evolution of material in the early Solar System ? 3. What are the physical properties and evolution of the building blocks of terrestrial planets ? 4. How do volatiles and organics in primitive NEAs relate to the atmosphere and life on Earth ? ESA CV M3 , 21 JAN. 2014 1. What was the astrophysical setting of the birth of the Solar System ? Eros, NEAR (NASA/JHU/APL) ESA CV M3 , 21 JAN. 2014 Fine–grained matrix hosting organics, volatiles Low temperature fine grained matrix Eros, NEAR (NASA/JHU/APL) ESA CV M3 , 21 JAN. 2014 Fine–grained matrix hosting organics, volatiles 1 µm PhotoESA CV M3 , 21 J : H. Leroux AN. 2014 Fine–grained matrix host grains of non-solar composition Presolar graphite SiC grains corundum Presolar diamond 2 nanometer scale transmission electron microscope image ESA CV M3 , 21 JAN. 2014 Credit : Univ. Chicago, MPI Mainz, Carnegie Inst. Wash Pre-solar grains that survived Solar System formation Presolar graphite SiC grains 105 AGB star grains Presolar SiC J-type C stars Mainstream Born-again AGB Type A&B 4 Type Y&Z 10 Type X Nova Unus./Type C N 103 15 solar N/ 14 102 corundum Presolar diamond 101 2 nanometer scale transmission Supernova grains electron microscope image Nova grains solar 100 10-1 100 101 102 103 104 12 13 C/ C Hoppe, 2010 ESA CV M3 , 21 JAN. 2014 Credit : Univ; Chicago, MPI Mainz, Carnegie Inst. Wash Insights into stellar nucleosynthesis AGB V838 Monocerotis Supernova 1987A Presolar grains provide information about nucleosynthesis and stellar evolution • Isotopic signatures of rapid neutron and alpha captures ALMA (ESO/NAOJ/NRAO) testing models of super- A. Angelich (NRAO/AUI/NSF) NASA, ESA and H.E. Bond (STScI) novae explosions (eg, 44Ca) • Insight into galactic evolution Tycho’s Nova Eta Carinae supernova (eg AGB stars) remnant • Physico-chemical conditions and events in stellar envelopes (eg red giants) NASA, ESA, HST NASA/MPIA/Calar Alto Obs., Oliver Krause et al. ESA CV M3 , 21 JAN. 2014 What are the links between past stars and the Solar System ? Supernova Proto-planetary disk Molecular Cloud Primitive asteroids AGB Star Lab analysis NASA, NEAR ESA CV M3 , 21 JAN. 2014 2. What is the origin and evolution of material in the early Solar System Ca - Al-rich inclusions (CAI) STARPLAN (10 µm - 2 cm) Eros, NEAR (NASA/JHU/APL) ESA CV M3 , 21 JAN. 2014 Extinct radioactivities : key tracers of early Solar System events 26 26 Al Mg (T1/2 = 0.7 Ma) 60 60 Fe Ni (T1/2 = 2.4 Ma) ESA CV M3 , 21 JAN. 2014 NGC 6357, Hester & Desch (2005) Extinct radioactivities : key tracers of proto-solar events Timing of Supernova explosions? Solar System protoplanetary disk ESA CV M3 , 21 JAN. 2014 Time scales of nebular vs. planetary processes • Radioisotope systems are susceptible to resetting during chondrules meteorite forming process • Samples of primitive unaltered material should significantly improve chronology CAIs ESA CV M3 , 21 JAN. 2014 3. What are the physical properties and evolution of the building blocks of terrestrial planets ? Regolith: the lunar soil legacy NASA Eros, NEAR (NASA/JHU/APL) ESA CV M3 , 21 JAN. 2014 A world in a grain : investigating asteroid processing in dust Cosmic-ray 0.5 µm produced Indigenous Volatiles (?) Radiogenic production Photo: Y. Langevin Amorphized skin NASA ESA CV M3 , 21 JSolar windAN. 2014 Non SW, surface-correlated A world in a grain : investigating asteroid processing in dust 0.5 µm Apollo soil grain 79035, 1 Ga 15N/14N +800 0 +400 δ D (‰) -100 0 D N(‰) 0 d 15 δ -200 -400 D/H -800 Solar 0 100 200 Depth below surface, nanometresNASA ESA CV M3 , 21 JAN. 2014 Hashizume et al., 2000 4a. How do organics in primitive NEAs relate to life on Earth ? The origin of life on Earth remains one of humankind’s important unanswered questions Organics from space Extraterrestrial delivery via small bodies seeded the young Earth during in its early history: precursor material for life ? P. Sawyert Smithsonian Early Earth’s chemistry ESA CV M3 , 21 JAN. 2014 Insights into cosmic carbon chemistry Interstellar and circumstellar regions : ~ 180 molecules are detected and many carbon allotropes …. Carbonaceous meteorites contain: macromolecular carbon, biomolecules, hydrocarbons, nanoglobules… Ehrenfreund et al. 2001 MarcoPolo-R will permit analysis of a unique sample of abiotic organic chemistry as it was in the Solar System shortly before the onset of life. ESA CV M3 , 21 JAN. 2014 4b. How do volatiles (H, C, N…) in primitive NEAs relate to the atmosphere and oceans on Earth ? Sun (Genesis) Busemann et al. 2006 Marty, 2012 • What are the compositions of asteroids ? Only measurements are from meteorites – possibility of terrestrial contamination • AreESA CV M3 , 21 J cometsAN. 2014 /asteroids the origin of terrestrial water and atmosphere ? A comet-asteroid continuum? Deep impact on Tempel1 Clays in meteorite 6 km 200 nm NASA/JPL-Caltech/UMD The computed water/rock ratio in meteorites (representative of asteroids?) is up to 1 (Clayton 1984, Young et al. 2002) The observed water/rock ratio of Comet Tempel 1 is 1 (A’Hearn et al. 2005) What is the difference between a water-rich asteroid & a dust-rich comet ? ESA CV M3 , 21 JAN. 2014 Why do we need to return samples when we have meteorites ? Atmospheric entry More than 99% of material lost in the atmosphere; only the <1% strongest survives Primitive OrDinary chonDrites material Chondrites CM Explosion of a cometary particle in Stardust 4 mm aerogel Atmospheric Entry Filter Compressive strength NASA Tsuchiyama et al. 2008 Carbonaceous chondrites are under-represented on Earth (5%) compared to the abundance of carbonaceous-type asteroids 32 ESA CV M3 , 21 JAN. 2014 Why do we need to return samples when we have meteorites ? Terrestrial contamination fall ! : a fresh Chelyabinsk ESA CV M3 , 21 JAN. 2014 Photo: Getty Why do we need to return samples when we have meteorites ? Tagish Lake Most perfectly collected meteorite to date? Collected within 5 days from frozen lake and kept at -20°C terrestrial contamination Terrestrial hydrocarbons … results obtained for organics in meteorites may Tagish Lake be questioned hydrocarbons 34 ESA CV M3 , 21 JAN.