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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.
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  • Ceres Is the Largest Object in the Asteroid Belt, Which Lies Mainly

    Ceres Is the Largest Object in the Asteroid Belt, Which Lies Mainly

    Dactyl, the moon of Ida, is shown below in a close-up and at its true size relative to Ida. Dactyl was the Ceres and the Asteroid Belt first asteroid moon to be discovered. Ceres is the largest object in the The best photos of Ceres (below left) and Vesta (below right) as As of 2008, only the asteroid belt, which lies mainly of 2008, from the Hubble Space Telescope (courtesy NASA/ESA) handful of asteroids between Mars and Jupiter. shown here have had Ida and Dactyl, from NASA’s Galileo Asteroids are made of various their pictures taken combinations of rocks, metals and by spacecraft flying carbon compounds that have past them. If you’re Steins, Ceres is much smaller than the Moon, which is shown below reading this panel from ESA’s Rosetta Eros, from NEAR never been captured by any after 2011, you’ve planet’s gravity. Asteroids have on the same scale as Ceres and Vesta above. Nonetheless, Shoemaker Ceres is sometimes referred to as a dwarf planet, hopefully seen better (NASA/JHUAPL) not changed much for billions of along with Pluto and a growing list of other objects. photos of Vesta, the years, making them important third-largest object in records of the formation of the the asteroid belt, solar system. The solar system taken by the Mathilde, from contains millions of asteroids Dawn spacecraft. And if you’re reading NEAR Shoemaker ranging down to the size of large (NASA/JHUAPL) this panel after 2015, boulders, as well as smaller hopefully there are objects called meteoroids.