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26 results on '"SOLAR-SYSTEM"'

1. Nano-FTIR spectroscopic identification of prebiotic carbonyl compounds in Dominion Range 08006 carbonaceous chondrite

Author

Bogdan Sava, Mehmet Yesiltas, and Timothy D. Glotch

Subjects
Science, Tagish Lake Meteorite, Context (language use), 02 engineering and technology, 010502 geochemistry & geophysics, 01 natural sciences, Characterization and analytical techniques, Parent body, Article, Petrography, Abiogenesis, Organic matter, 0105 earth and related environmental sciences, chemistry.chemical_classification, Metamorphism, Aldehydes, Minerals, Multidisciplinary, Carboxylic-Acids, Extraterrestrial materials, Spectra, Insoluble Organic-Matter, 021001 nanoscience & nanotechnology, Astrobiology, Grains, chemistry, Chemical engineering, Meteorite, Carbonaceous chondrite, Meteoritics, Medicine, Solar-System, 0210 nano-technology, Infrared-Spectroscopy
Abstract

Meteorites contain organic matter that may have contributed to the origin of life on Earth. Carbonyl compounds such as aldehydes and carboxylic acids, which occur in meteorites, may be precursors of biologically necessary organic materials in the solar system. Therefore, such organic matter is of astrobiological importance and their detection and characterization can contribute to the understanding of the early solar system as well as the origin of life. Most organic matter is typically sub-micrometer in size, and organic nanoglobules are even smaller (50-300 nm). Novel analytical techniques with nanoscale spatial resolution are required to detect and characterize organic matter within extraterrestrial materials. Most techniques require powdered samples, consume the material, and lose petrographic context of organics. Here, we report the detection of nanoglobular aldehyde and carboxylic acids in a highly primitive carbonaceous chondrite (DOM 08006) with similar to 20 nm spatial resolution using nano-FTIR spectroscopy. Such organic matter is found within the matrix of DOM 08006 and is typically 50-300 nm in size. We also show petrographic context and nanoscale morphologic/topographic features of the organic matter. Our results indicate that prebiotic carbonyl nanoglobules can form in a less aqueous and relatively elevated temperature-environment (220-230 degrees C) in a carbonaceous parent body. RISE2 node of NASA's Solar System Exploration Research Virtual Institute (SSERVI) We thank the associate editor and the reviewers for their constructive comments, which significantly improved this manuscript. We thank NASA-JSC for providing the meteorite samples. This work was also supported in part by the RISE2 node of NASA's Solar System Exploration Research Virtual Institute (SSERVI; PI: T.D. Glotch).

Published
2021

2. Timing of thermal metamorphism in CM chondrites: Implications for Ryugu and Bennu future sample return

Author

Frédéric Moynier, Elsa Amsellem, Pierre Beck, Brandon Mahan, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Inst Univ France, F-75005 Paris, France, Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Macquarie Univ, Dept Earth & Planetary Sci, Sydney, NSW 2109, Australia, ‎ Inst Univ France, Paris, France, and Univ Grenoble Alpes, Inst Planetol & Astrophys Grenoble, CNES, CNRS, F-38000 Grenoble, France

Subjects
Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, 01 natural sciences, Astrobiology, SOLAR-SYSTEM, Chondrite, 0103 physical sciences, EARTH, ASTEROID FAMILIES, ISOTOPIC COMPOSITION, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), RB-SR, METEORITES, Astronomy and Astrophysics, KeyWords Plus:CARBONACEOUS CHONDRITES, CI, Astrophysics - Astrophysics of Galaxies, Meteorite, AQUEOUS ALTERATION, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), VOLATILE LOSS, Terrestrial planet, Formation and evolution of the Solar System, Geology, Radioactive decay, Earth (classical element), Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; Carbonaceous chondrites are often considered potential contributors of water and other volatiles to terrestrial planets as most of them contain significant amounts of hydrous mineral phases. As such, carbonaceous chondrites are candidate building blocks for Earth, and elucidating their thermal histories is of direct importance for understanding the volatile element history of Earth and the terrestrial planets. A significant fraction of CM type carbonaceous chondrites are thermally metamorphosed or "heated" and have lost part of their water content. The origin and the timing of such heating events are still debated, as they could have occurred either in the first Myrs of the Solar System via short-lived radioactive heating, or later by impact induced heating and/or solar radiation. Since Rb is more volatile than Sr, and some heated CM chondrites are highly depleted in Rb, a dating system based on the radioactive decay of Rb-87 to( 87)Sr(lambda(87) Rb = 1.393 x 10(-11) yr(-1)) could be used to date the heating event relating to the fractionation of Rb and Sr. Here, we have leveraged the Rb-87/Sr-87 system to date the heating of five CM chondrites (PCA 02012, PCA 02010, PCA 91008, QUE 93005 and MIL 07675). We find that the heating events of all five meteorites occurred at least 3 Ga after the formation of the Solar System. Such timing excludes short-lived radioactive heating as the origin of thermal metamorphism in these meteorites, and relates such heating events to ages of collisional families of C-type asteroids.

Published
2020

3. Was Planet 9 captured in the Sun’s natal star-forming region?

Author

Tim Lichtenberg, Sascha P. Quanz, Richard J. Parker, and Astronomy

Subjects
Solar System, planets and satellites: dynamical evolution and stability, stars: kinematics and dynamics, FOS: Physical sciences, POPULATION SYNTHESIS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, MASS, Star (graph theory), numerical, open clusters and associations: general [methods], 01 natural sciences, methods: numerical, SOLAR-SYSTEM, Physics - Geophysics, BINARIES, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, DYNAMICAL EVOLUTION, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Star formation, Astronomy and Astrophysics, open clusters and associations: general, Astrophysics - Astrophysics of Galaxies, Geophysics (physics.geo-ph), Stars, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Protoplanetary disc, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, SURVIVAL, SUPERNOVA ENRICHMENT, Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System, CLUSTERS, Astrophysics - Earth and Planetary Astrophysics
Abstract

The presence of an unseen ‘Planet 9’ on the outskirts of the Solar system has been invoked to explain the unexpected clustering of the orbits of several Edgeworth–Kuiper Belt Objects. We use N-body simulations to investigate the probability that Planet 9 was a free-floating planet (FFLOP) that was captured by the Sun in its birth star formation environment. We find that only 1–6 per cent of FFLOPs are ensnared by stars, even with the most optimal initial conditions for capture in star-forming regions (one FFLOP per star, and highly correlated stellar velocities to facilitate capture). Depending on the initial conditions of the star-forming regions, only 5–10 of 10 000 planets are captured on to orbits that lie within the constraints for Planet 9. When we apply an additional environmental constraint for Solar system formation – namely the injection of short-lived radioisotopes into the Sun’s protoplanetary disc from supernovae – we find the probability for the capture of Planet 9 to be almost zero., Monthly Notices of the Royal Astronomical Society. Letters, 472 (1), ISSN:1745-3933, ISSN:1745-3925

Published
2019

4. Compositional distributions and evolutionary processes for the near-Earth object population : Results from the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS)

Author

Alan T. Tokunaga, Michael D. Hicks, Vishnu Reddy, David Polishook, M. Birlan, R. P. Binzel, Francesca E. DeMeo, Tomas Kohout, Juan A. Sanchez, B. Burt, Cristina A. Thomas, N. Moskovitz, Emma V. Turtelboom, T. L. Dunn, Alessandro Morbidelli, S. M. Slivan, Benoit Carry, Mikael Granvik, Pierre Vernazza, C. Lantz, Thomas H. Burbine, S. J. Bus, Andrew S. Rivkin, Staff Services, Particle Physics and Astrophysics, Planetary-system research, Department of Geosciences and Geography, Geology and Geophysics, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institute for Astronomy [Honolulu], University of Hawai'i [Honolulu] (UH), Department of Astronomy of the Mount Holyoke College, Mount Holyoke College, Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), UND Department of Space Studies, University of North Dakota [Grand Forks] (UND), Laboratorio de Biología Molecular Marina (BIOMMAR), Universidad de los Andes [Bogota] (UNIANDES), Smithsonian Institution-Harvard University [Cambridge], Beverly and Raymond Sackler Faculty of Exact Sciences, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Helsinki, Staff Services, and University of Helsinki, Department of Geosciences and Geography

Subjects
Solar System, 010504 meteorology & atmospheric sciences, SPECTRAL PROPERTIES, Population, FRESH SURFACES, FOS: Physical sciences, Astrophysics, PYROXENE MIXTURES, 01 natural sciences, Space weathering, SOLAR-SYSTEM, Planet, Chondrite, 0103 physical sciences, education, SOURCE REGIONS, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), PARENT BODY, education.field_of_study, Near-Earth object, Potentially hazardous object, Astronomy and Astrophysics, REFLECTANCE SPECTRA, 15. Life on land, ORDINARY CHONDRITES, 115 Astronomy, Space science, ASTEROID PAIRS, 13. Climate action, Space and Planetary Science, Asteroid, MAIN-BELT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

Advancing technology in near-infrared instrumentation and dedicated planetary telescope facilities have enabled nearly two decades of reconnoitering the spectral properties for near-Earth objects (NEOs). We report measured spectral properties for more than 1000 NEOs, representing >5% of the currently discovered population. Thermal flux detected below 2.5 µm allows us to make albedo estimates for nearly 50 objects, including two comets. Additional spectral data are reported for more than 350 Mars-crossing asteroids. Most of these measurements were achieved through a collaboration between researchers at the Massachusetts Institute of Technology and the University of Hawaii, with full cooperation of the NASA Infrared Telescope Facility (IRTF) on Mauna Kea. We call this project the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS; myth-neos). While MITHNEOS has continuously released all spectral data for immediate use by the scientific community, our objectives for this paper are to: (1) detail the methods and limits of the survey data, (2) formally present a compilation of results including their taxonomic classification within a single internally consistent framework, (3) perform a preliminary analysis on the overall population characteristics with a concentration toward deducing key physical processes and identifying their source region for escaping the main belt. Augmenting our newly published measurements are the previously published results from the broad NEO community, including many results graciously shared by colleagues prior to formal publication. With this collective data set, we find the near-Earth population matches the diversity of the main-belt, with all main-belt taxonomic classes represented in our sample. Potentially hazardous asteroids (PHAs) as well as the subset of mission accessible asteroids (ΔV ≤ 7 km/s) both appear to be a representative mix of the overall NEO population, consistent with strong dynamical mixing for the population that interacts most closely with Earth. Mars crossers, however, are less diverse and appear to more closely match the inner belt population from where they have more recently diffused. The fractional distributions of major taxonomic classes (60% S, 20% C, 20% other) appear remarkably constant over two orders of magnitude in size (10 km to 100 m), which is eight orders of magnitude in mass, though we note unaccounted bias effects enter into our statistics below about 500 m. Given the range of surface ages, including possible refreshment by planetary encounters, we are able to identify a very specific space weathering vector tracing the transition from Q- to Sq- to S-types that follows the natural dispersion for asteroid spectra mapped into principal component space. We also are able to interpret a shock darkening vector that may account for some objects having featureless spectra. Space weathering effects for C-types are complex; these results are described separately by Lantz, Binzel, DeMeo. (2018, Icarus 302, 10–17). Independent correlation of dynamical models with taxonomic classes map the escape zones for NEOs to main-belt regions consistent with well established heliocentric compositional gradients. We push beyond taxonomy to interpret our visible plus near-infrared spectra in terms of the olivine and pyroxene mineralogy consistent with the H, L, and LL classes of ordinary chondrites meteorites. Correlating meteorite interpretations with dynamical escape region models shows a preference for LL chondrites to arrive from the ν6 resonance and H chondrites to have a preferential signature from the mid-belt region (3:1 resonance). L chondrites show some preference toward the outer belt, but not at a significant level. We define a Space Weathering Parameter as a continuous variable and find evidence for step-wise changes in space weathering properties across different planet crossing zones in the inner solar system. Overall we hypothesize the relative roles of planetary encounters, YORP spin-up, and thermal cycling across the inner solar system.

Published
2019

5. Micrometeorites: Insights into the flux, sources and atmospheric entry of extraterrestrial dust at Earth

Author

M. D. Suttle, Matthias Van Ginneken, Matthew J. Genge, and Science and Technology Facilities Council (STFC)

Subjects
Solar System, Meteors, 010504 meteorology & atmospheric sciences, TRANSANTARCTIC MOUNTAINS, Weathering, Astronomy & Astrophysics, 01 natural sciences, OXYGEN, Astrobiology, ACCRETION RATE, SOLAR-SYSTEM, Interplanetary dust cloud, Chondrite, ANTARCTIC MICROMETEORITES, Interplanetary dust, 0201 Astronomical and Space Sciences, 0103 physical sciences, Comets, ISOTOPIC COMPOSITIONS, Micrometeorites, 010303 astronomy & astrophysics, QE515, 0105 earth and related environmental sciences, Science & Technology, Meteoroid, FINE-GRAINED MICROMETEORITES, Astronomy and Astrophysics, COMET 81P/WILD-2, Snow, Asteroids, Deposition (aerosol physics), Space and Planetary Science, COSMIC SPHERULES, Extraterrestrial life, Physical Sciences, CHONDRITIC MICROMETEORITES, Environmental science
Abstract

Micrometeorites (MMs) provide constraints on the flux and sources of extraterrestrial dust falling on Earth as well as recording the processes occurring during atmospheric entry. Collections of micrometeorites have been recovered from a wide variety of environments including Antarctic moraine, rock traps, ice and snow and on roof tops in urban areas. Studies of the mineralogy and composition of MMs suggest that most particles (>98%) >50 ​μm in diameter have asteroidal sources, whilst ~50% of particles smaller than 50 ​μm are likely to be derived from comets. The relative abundance of S(IV)-type asteroid materials, similar to ordinary chondrites increases with size, although C-type asteroidal materials, similar to carbonaceous chondrites dominate over all. Although MMs provide excellent evidence on the nature and abundance of extraterrestrial dust at the Earth’s orbit they are not without bias and uncertainty. Mineralogical and compositional change during atmospheric entry makes the exact nature of their precursors uncertain complicating evaluation of source beyond basic classes of material. This is particularly true at larger sizes when complete melting to form cosmic spherules occurs, however, unmelted MMs >50 ​μm in size are also often thermally altered. Mixing with atmospheric oxygen and mass fractionation by evaporation furthermore complicates the use of oxygen isotope compositions in identifying parent bodies. All MM collections are suggested to exhibit biases owing to: (1) collection method, (2) terrestrial weathering, (3) terrestrial contamination, and (4) erosion and deposition by terrestrial surface processes. Even in the least biased collections, those collected by dedicated melting of Antarctic snow, erosive loss of material is suggested here to make fluxes uncertain by factors of up to ~2. The abundance of asteroid-derived MMs observed in collections contradicts models of the orbital evolution of interplanetary dust to Earth, which suggests >70% should be provided by comets.

Published
2020

6. CASTAway: An asteroid main belt tour and survey

Author

Henning Haack, Nicolas Thomas, Joan Pau Sánchez, J. de León, Andreas Nathues, Francesca E. DeMeo, Aurelie Guilbert-Lepoutre, A. Gibbings, Ian Thomas, Ákos Kereszturi, Fraser Clarke, Neil Bowles, Tristram Warren, C. M. Marriner, J. Leif Jorgensen, Matthias Tecza, V. Da Deppo, Naomi Murdoch, Alena Probst, Paul Eccleston, Andrew S. Rivkin, Ian Tosh, Sonia Fornasier, Thomas Andert, P. Pravec, K. L. Donaldson Hanna, Jessica A. Arnold, Mikael Granvik, Kjartan M. Kinch, Enzo Pascale, Benoit Carry, Ann Carine Vandaele, Colin Snodgrass, Giampiero Naletto, John K. Davies, Benjamin T. Greenhagen, Rhian H. Jones, Katherine H. Joy, Simon F. Green, Jessica Agarwal, Javier Licandro, J.M. Barnes, Laurent Jorda, Manish R. Patel, S. B. Calcutt, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Department of Mechanical and Aerospace Engineering [Glasgow], University of Strathclyde, Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Institut für Raumfahrttechnik, Universität der Bundeswehr München [Neubiberg] = Bundeswehr University, Laboratoire des Mécanismes et Transfert en Géologie (LMTG), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), FIME, Universidad Autonoma de Nuevo leon, Universidad Autonoma de Madrid (UAM), Institut universitaire des systèmes thermiques industriels (IUSTI), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Collegium Budapest (Institute for Advanced Study) (CB), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (ASCR), Vetco Gray (VG), Vetco Gray, Cardiff University, Instituto de Astrofisica de Canarias (IAC), University of Oxford [Oxford], Department of Physics, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Universität der Bundeswehr München [Neubiberg]

Subjects
[SPI.OTHER]Engineering Sciences [physics]/Other, Atmospheric Science, Solar System, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], CERES, 7. Clean energy, 01 natural sciences, Star tracker, law.invention, Astrobiology, MAGNITUDE, Autre, law, P/2010 A2, SPACE-TELESCOPE, Survey, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), SPECTROSCOPY, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Remote sensing, Main Asteroid Belt, survey, flyby, mapping, remote sensing, Geophysics, Mapping, Asteroid, Asteroid belt, ROSETTA, Geology, SURFACE, Flyby, Aerospace Engineering, Space and Planetary Science, FOS: Physical sciences, Context (language use), Telescope, SOLAR-SYSTEM, 0103 physical sciences, 0105 earth and related environmental sciences, 21 LUTETIA, Spacecraft, business.industry, Payload, ICE, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, 13. Climate action, General Earth and Planetary Sciences, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

CASTAway is a mission concept to explore our Solar System's main asteroid belt. Asteroids and comets provide a window into the formation and evolution of our Solar System and the composition of these objects can be inferred from space-based remote sensing using spectroscopic techniques. Variations in composition across the asteroid populations provide a tracer for the dynamical evolution of the Solar System. The mission combines a long-range (point source) telescopic survey of over 10,000 objects, targeted close encounters with 10 to 20 asteroids and serendipitous searches to constrain the distribution of smaller (e.g. 10 m) size objects into a single concept. With a carefully targeted trajectory that loops through the asteroid belt, CASTAway would provide a comprehensive survey of the main belt at multiple scales. The scientific payload comprises a 50 cm diameter telescope that includes an integrated low-resolution (R = 30 to 100) spectrometer and visible context imager, a thermal (e.g. 6 to 16 microns) imager for use during the flybys, and modified star tracker cameras to detect small (approx. 10 m) asteroids. The CASTAway spacecraft and payload have high levels of technology readiness and are designed to fit within the programmatic and cost caps for a European Space Agency medium class mission, whilst delivering a significant increase in knowledge of our Solar System., 40 pages, accepted by Advances in Space Research October 2017

Published
2018

7. Debiased orbit and absolute-magnitude distributions for near-Earth objects

Author

Patrick Michel, Alessandro Morbidelli, E. C. Beshore, David Vokrouhlický, William F. Bottke, Bryce Bolin, Robert Jedicke, Mikael Granvik, David Nesvorný, Department of Physics, Planetary-system research, Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), University of Arizona, and Charles University [Prague] (CU)

Subjects
Absolute magnitude, Solar System, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, ASTEROID BELT, Near-Earth objects, 01 natural sciences, SOLAR-SYSTEM, Orbital, 0103 physical sciences, Comets, COLLISION PROBABILITY, HIGH-INCLINATION ORBITS, JUPITER-FAMILY COMETS, SIZE-FREQUENCY DISTRIBUTION, Eccentricity (behavior), education, 010303 astronomy & astrophysics, POPULATION, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Near-Earth object, Astronomy, Astronomy and Astrophysics, HAZARD, 115 Astronomy, Space science, Asteroids, Dynamics, MODEL, Orbit, 13. Climate action, Space and Planetary Science, Asteroid, Resonances, Physics::Space Physics, Asteroid belt, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The debiased absolute-magnitude and orbit distributions as well as source regions for near-Earth objects (NEOs) provide a fundamental frame of reference for studies of individual NEOs and more complex population-level questions. We present a new four-dimensional model of the NEO population that describes debiased steady-state distributions of semimajor axis, eccentricity, inclination, and absolute magnitude $H$ in the range $17, Comment: 33 pages, 28 figures, accepted for publication in Icarus

Published
2018

8. OSSOS. VII. 800+ Trans-Neptunian Objects—The Complete Data Release

Author

Pierre Vernazza, Sarah Greenstreet, Cory Shankman, Michael Marsset, Wing-Huen Ip, Rebekah I. Dawson, Ruth Murray-Clay, Marian Jakubik, Rosemary E. Pike, Michele T. Bannister, Pedro Lacerda, Audrey Thirouin, Patryk Sofia Lykawka, Brett Gladman, Matthew J. Lehner, Mike Alexandersen, Christa Van Laerhoven, Hsing Wen Lin, Aurélie Guilbert-Lepoutre, Mikael Granvik, Kathryn Volk, R. Lynne Jones, Samantha Lawler, Susan D. Benecchi, Nahuel Cabral, Audrey Delsanti, Stephen D. J. Gwyn, Megan E. Schwamb, Nathan A. Kaib, Shiang-Yu Wang, Jean-Marc Petit, Philippe Rousselot, Ying-Tung Chen, J. J. Kavelaars, Edward Ashton, Wesley C. Fraser, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki-University of Helsinki, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Lowell Observatory [Flagstaff], Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Department of Physics

Subjects
Solar System, 010504 meteorology & atmospheric sciences, MIGRATION, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, KUIPER-BELT OBJECTS, Ephemeris, NEPTUNE, 01 natural sciences, SOLAR-SYSTEM, surveys, Neptune, 0103 physical sciences, Trans-Neptunian object, education, 010303 astronomy & astrophysics, Minor planet, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, JUPITER, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, TROJANS, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ORIGIN, Giant planet, Astronomy, Astronomy and Astrophysics, general [Kuiper belt], RESONANCE, 115 Astronomy, Space science, Orbit, URANUS, 13. Climate action, Space and Planetary Science, DISCOVERY, Kuiper belt: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

The Outer Solar System Origins Survey (OSSOS), a wide-field imaging program in 2013-2017 with the Canada-France-Hawaii Telescope, surveyed 155 deg$^{2}$ of sky to depths of $m_r = 24.1$-25.2. We present 838 outer Solar System discoveries that are entirely free of ephemeris bias. This increases the inventory of trans-Neptunian objects (TNOs) with accurately known orbits by nearly 50%. Each minor planet has 20-60 Gaia/Pan-STARRS-calibrated astrometric measurements made over 2-5 oppositions, which allows accurate classification of their orbits within the trans-Neptunian dynamical populations. The populations orbiting in mean-motion resonance with Neptune are key to understanding Neptune's early migration. Our 313 resonant TNOs, including 132 plutinos, triple the available characterized sample and include new occupancy of distant resonances out to semi-major axis $a \sim 130$ au. OSSOS doubles the known population of the non-resonant Kuiper belt, providing 436 TNOs in this region, all with exceptionally high-quality orbits of $a$ uncertainty $\sigma_{a} \leq 0.1\%$; they show the belt exists from $a \gtrsim 37$ au, with a lower perihelion bound of $35$ au. We confirm the presence of a concentrated low-inclination $a\simeq 44$ au "kernel" population and a dynamically cold population extending beyond the 2:1 resonance. We finely quantify the survey's observational biases. Our survey simulator provides a straightforward way to impose these biases on models of the trans-Neptunian orbit distributions, allowing statistical comparison to the discoveries. The OSSOS TNOs, unprecedented in their orbital precision for the size of the sample, are ideal for testing concepts of the history of giant planet migration in the Solar System., Comment: Invited paper, special issue Data: Insights and Challenges in a Time of Abundance. Data tables and example survey simulator are in the supplementary materials (see arXiv source under Downloads > Other formats)

Published
2018

9. X-ray radiative transfer in protoplanetary disks

Author

Manuel Güdel, Wing-Fai Thi, Rowin Meijerink, Inga Kamp, Ch. Rab, Giambattista Aresu, Michiel Min, Peter Woitke, Astronomy, Low Energy Astrophysics (API, FNWI), European Commission, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
X-ray background, Astrophysics, Protoplanetary disk, 01 natural sciences, Luminosity, Radiative transfer, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, formation [Stars], QC, Astrochemistry, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), astrochemistry, PHOTOIONIZATION CROSS-SECTIONS, Circumstellar matter, OPTICAL-PROPERTIES, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, radiative transfer, Astrophysics::Earth and Planetary Astrophysics, MWC 480, INTERSTELLAR DUST, ANALYTIC FITS, T-TAURI STARS, LINE EMISSION, Astrophysics::High Energy Astrophysical Phenomena, NDAS, FOS: Physical sciences, circumstellar matter, PHOTOELECTRIC-EMISSION, methods: numerical, SOLAR-SYSTEM, 0103 physical sciences, 010306 general physics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Cosmic dust, numerical [Methods], stars: formation, Astronomy and Astrophysics, YOUNG STELLAR OBJECTS, Astrophysics - Astrophysics of Galaxies, Stars, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Earth and Planetary Astrophysics
Abstract

The X-ray luminosities of T Tauri stars are about two to four orders of magnitude higher than the luminosity of the contemporary Sun. As these stars are born in clusters, their disks are not only irradiated by their parent star but also by an X-ray background field produced by the cluster members. We aim to quantify the impact of X-ray background fields produced by young embedded clusters on the chemical structure of disks. Further, we want to investigate the importance of the dust for X-ray radiative transfer in disks. We present a new X-ray radiative transfer module for the radiation thermo-chemical disk code ProDiMo, which includes X-ray scattering and absorption by both the gas and dust component. For the X-ray radiative transfer, we consider irradiation by the star and by X-ray background fields. To study the impact of X-rays on the chemical structure of disks we use the well-established disk ionization tracers N2H+ and HCO+. For evolved dust populations, X-ray opacities are mostly dominated by the gas; only for photon energies $E\gtrsim5-10\,$keV, dust opacities become relevant. Consequently, the local disk X-ray radiation field is only affected in dense regions close to the disk midplane. X-ray background fields can dominate the local X-ray disk ionization rate for disk radii $r\gtrsim20\,$au. However, the N2H+ and HCO+ column densities are only significantly affected in case of low cosmic-ray ionization rates, or if the background flux is at least a factor of ten higher than the flux level expected for clusters typical for the solar vicinity. Observable signatures of X-ray background fields in low-mass star-formation regions, like Taurus, are only expected for cluster members experiencing a strong X-ray background field. For the majority of the cluster members, the X-ray background field has only little impact on the disk chemical structure., 16 pages, 12 figures, accepted for publication in A&A

Published
2018

10. Late metal–silicate separation on the IAB parent asteroid: constraints from combined W and Pt isotopes and thermal modelling

Author

A. C. Hunt, Philip M. Reger, Maria Schönbächler, David L. Cook, Mattias Ek, Tim Lichtenberg, Gregor J. Golabek, and Astronomy

Subjects
multi-collector ICP-MS, CORE FORMATION, Planetesimal, WINONAITES, FOS: Physical sciences, Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, Parent body, Astrobiology, SOLAR-SYSTEM, Physics - Geophysics, chemistry.chemical_compound, Geochemistry and Petrology, IAB iron meteorites, Hf–W chronometry, Pt isotopes, Planetesimals, Thermal histories, 0103 physical sciences, IRON-METEORITE COMPLEX, Earth and Planetary Sciences (miscellaneous), Hf-W chronometry, thermal histories, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Isotope, PLATINUM ISOTOPES, Silicate, MANTLE DIFFERENTIATION, Geophysics (physics.geo-ph), OXYGEN-ISOTOPE, EXPOSURE AGES, Neutron capture, Geophysics, Meteorite, chemistry, 13. Climate action, Space and Planetary Science, Asteroid, NEUTRON-CAPTURE, RAPID ACCRETION, Internal heating, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

The short-lived $^{182}$Hf-$^{182}$W decay system is a powerful chronometer for constraining the timing of metal-silicate separation and core formation in planetesimals and planets. Neutron capture effects on W isotopes, however, significantly hamper the application of this tool. In order to correct for neutron capture effects, Pt isotopes have emerged as a reliable in-situ neutron dosimeter. This study applies this method to IAB iron meteorites, in order to constrain the timing of metal segregation on the IAB parent body. The $\epsilon^{182}$W values obtained for the IAB iron meteorites range from -3.61 $\pm$ 0.10 to -2.73 $\pm$ 0.09. Correlating $\epsilon^{\mathrm{i}}$Pt with $^{182}$W data yields a pre-neutron capture $^{182}$W of -2.90 $\pm$ 0.06. This corresponds to a metal-silicate separation age of 6.0 $\pm$ 0.8 Ma after CAI for the IAB parent body, and is interpreted to represent a body-wide melting event. Later, between 10 and 14 Ma after CAI, an impact led to a catastrophic break-up and subsequent reassembly of the parent body. Thermal models of the interior evolution that are consistent with these estimates suggest that the IAB parent body underwent metal-silicate separation as a result of internal heating by short-lived radionuclides and accreted at around 1.4 $\pm$ 0.1 Ma after CAIs with a radius of greater than 60 km., Comment: 11 pages, 8 figures, 2 tables; open access article under the CC BY-NC-ND license (see http://creativecommons.org/licenses/by-nc-nd/4.0/)

Published
2017

11. s-Processing from MHD-induced mixing and isotopic abundances in presolar SiC grains

Author

Sara Palmerini, Oscar Trippella, Azzurra Zucchini, Maurizio Petrelli, Maurizio Busso, Diego Vescovi, and Francesco Frondini

Subjects
Red giant, ASYMPTOTIC-GIANT-BRANCH, SILICON-CARBIDE GRAINS, MAGNETIC-FIELDS, AGB STARS, SOLAR-SYSTEM, STELLAR EVOLUTION, OPEN CLUSTERS, CARBON STARS, MASS STARS, RED GIANT, FOS: Physical sciences, Natural abundance, Astrophysics, 01 natural sciences, Geochemistry and Petrology, Nucleosynthesis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Asymptotic giant branch, 010303 astronomy & astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Carbon star, Stars, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Low Mass
Abstract

In the past years the observational evidence that s-process elements from Sr to Pb are produced by stars ascending the socalled Asymptotic Giant Branch (or AGB) could not be explained by self-consistent models, forcing researchers to extensive parameterizations. The crucial point is to understand how protons can be injected from the envelope into the He-rich layers, yielding the formation of 13C and then the activation of the 13C(a,n)16O reaction. Only recently, attempts to solve this problem started to consider quantitatively physically-based mixing mechanisms. Among them, MHD processes in the plasma were suggested to yield mass transport through magnetic buoyancy. In this framework, we compare results of nucleosynthesis models for Low Mass AGB Stars (M, 16 page, 10 figures

Published
2017

12. In Situ Analysis of Non-Traditional Isotopes by SIMS and LA–MC–ICP–MS: Key Aspects and the Example of Mg Isotopes in Olivines and Silicate Glasses

Author

Zhengbin Deng, Julien Moureau, Frank M. Richter, Frédéric Moynier, Johan Villeneuve, Marc Chaussidon, Bruce Watson, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY 12180 USA, Univ Chicago, 5734 South Ellis Ave, Chicago, IL 60637 USA, and This work was supported by the UnivEarthS Labex program (ANR-10-LABX-0023 and ANR-11-IDEX-0005–02) and by ANR grant ANR grant CRADLE (ANR-15-CE31-0004-01).

Subjects
Analytical chemistry, Geochemistry, Fractionation, U-PB, 010502 geochemistry & geophysics, 01 natural sciences, SOLUTION NEBULIZATION, SOLAR-SYSTEM, chemistry.chemical_compound, Geochemistry and Petrology, TRACE-ELEMENT ABUNDANCES, 0105 earth and related environmental sciences, Isotope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Chemistry, Stable isotope ratio, 010401 analytical chemistry, FEMTOSECOND LASER-ABLATION, MASS-SPECTROMETRY, Silicate, 0104 chemical sciences, ION MICROPROBE ANALYSIS, Planetary science, 13. Climate action, [SDU]Sciences of the Universe [physics], Igneous differentiation, FRACTIONATION LAWS, Radioactive decay, Earth (classical element), KeyWords Plus:INDUCTIVELY-COUPLED-PLASMA, EXCIMER-LASER
Abstract

Isotopic variation for traditional elements (H, C, N, O and S) has been widely used in the past 40 years in Earth and planetary sciences to study many processes with an emphasis on environments where fluids are present (e.g., Valley and Cole 2011). More recent developments have allowed high-precision measurements of isotope ratios of what has been called non-traditional elements (i.e., Mg, Si, Fe, Zn, Cu, Mo), which are usually less fractionated than traditional elements by at least an order of magnitude (see this volume). These non-traditional stable isotopes can give insights on processes where fluids are not present (e.g., metal–silicate fractionation, e.g., Georg et al. 2007 and review by Poitrasson et al. 2017, this volume), evaporation processes during planetary formation (e.g., Paniello et al. 2012, Wang and Jacobsen 2016, and review by Moynier et al. 2017 this volume), igneous differentiation (e.g., Williams et al. 2009; Sossi et al. 2012; and review by Dauphas et al. 2017, this volume), and on biological processes (e.g., Walczyk and von Blanckenburg 2002, and review by Albarede et al. 2017 this volume). Among all these non-traditional isotopic systems, Mg isotopes are of major importance because (i) Mg is a major constituent of the silicate portion of planetary bodies, (ii) Mg has more than two isotopes (24Mg, 25Mg and 26Mg) allowing to study processes leading to various types of mass fractionation (Young et al. 2002; Young and Galy 2004; Davis et al. 2015) and (iii) 26Mg excesses produced by the radioactive decay of short-lived 26Al (T1/2=0.73 Ma) (Lee et al. 1976) are a key tool for early Solar system chronology (see reviews by Dauphas and Chaussidon 2011; Chaussidon and Liu 2015). Note that in addition, significant Mg isotopic …

Published
2017

13. A geochemical study of the winonaites: Evidence for limited partial melting and constraints on the precursor composition

Author

A. C. Hunt, Katharina Kreissig, Philip A. Bland, Mark Rehkämper, Gretchen Benedix, Stanislav Strekopytov, Samantha J. Hammond, and Science and Technology Facilities Council (STFC)

Subjects
Geochemistry & Geophysics, FORSTERITE CHONDRITES, 010504 meteorology & atmospheric sciences, Primitive achondrite, Geochemistry, Mineralogy, Precursor material, CHEMICAL-ANALYSES, 010502 geochemistry & geophysics, 01 natural sciences, Parent body, LODRANITE PARENT BODY, Metal-silicate separation, SOLAR-SYSTEM, chemistry.chemical_compound, ACHONDRITES, Geochemistry and Petrology, Chondrite, IAB iron meteorite, ICP-MS, 0402 Geochemistry, Achondrite, 0105 earth and related environmental sciences, IAB IRON-METEORITES, Science & Technology, Partial melting, Winonaite, Silicate, EVOLUTION, SILICATE INCLUSIONS, OXYGEN-ISOTOPE, STONY METEORITES, chemistry, Meteorite, 0403 Geology, Physical Sciences, Geology
Abstract

The winonaites are primitive achondrites which are associated with the IAB iron meteorites. Textural evidence implies heating to at least the Fe, Ni–FeS cotectic, but previous geochemical studies are ambiguous about the extent of silicate melting in these samples. Oxygen isotope evidence indicates that the precursor material may be related to the carbonaceous chondrites. Here we analysed a suite of winonaites for modal mineralogy and bulk major- and trace-element chemistry in order to assess the extent of thermal processing as well as constrain the precursor composition of the winonaite-IAB parent asteroid.\ud \ud Modal mineralogy and geochemical data are presented for eight winonaites. Textural analysis reveals that, for our sub-set of samples, all except the most primitive winonaite (Northwest Africa 1463) reached the Fe, Ni–FeS cotectic. However, only one (Tierra Blanca) shows geochemical evidence for silicate melting processes. Tierra Blanca is interpreted as a residue of small-degree silicate melting. Our sample of Winona shows geochemical evidence for extensive terrestrial weathering. All other winonaites studied here (Fortuna, Queen Alexander Range 94535, Hammadah al Hamra 193, Pontlyfni and NWA 1463) have chondritic major-element ratios and flat CI-normalised bulk rare-earth element patterns, suggesting that most of the winonaites did not reach the silicate melting temperature. The majority of winonaites were therefore heated to a narrow temperature range of between ∼1220 (the Fe, Ni–FeS cotectic temperature) and ∼1370 K (the basaltic partial melting temperature). Silicate inclusions in the IAB irons demonstrate partial melting did occur in some parts of the parent body (Ruzicka and Hutson, 2010), thereby implying heterogeneous heat distribution within this asteroid. Together, this indicates that melting was the result of internal heating by short-lived radionuclides. The brecciated nature of the winonaites suggests that the parent body was later disrupted by a catastrophic impact, which allowed the preservation of the largely unmelted winonaites.\ud \ud Despite major-element similarities to both ordinary and enstatite chondrites, trace-element analysis suggests the winonaite parent body had a carbonaceous chondrite-like precursor composition. The parent body of the winonaites was volatile-depleted relative to CI, but enriched compared to the other carbonaceous classes. The closest match are the CM chondrites; however, the specific precursor is not sampled in current meteorite collections.

Published
2017

14. REALISTIC DETECTABILITY OF CLOSE INTERSTELLAR COMETS

Author

Mikael Granvik, Nathaniel V. Cook, Darin Ragozzine, Denise C. Stephens, Department of Physics, and Planetary-system research

Subjects
Planetesimal, Solar System, 010504 meteorology & atmospheric sciences, Population, INNER OORT CLOUD, FOS: Physical sciences, KUIPER-BELT OBJECTS, Ephemeris, 01 natural sciences, SOLAR-SYSTEM, Planet, EXTRASOLAR COMETS, 0103 physical sciences, PLANETARY SYSTEMS, SIZE DISTRIBUTION, education, C/2007 W1 BOATTINI, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ISM: general, Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, comets: general, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Galaxy, 13. Climate action, Space and Planetary Science, Interstellar comet, BETA-PICTORIS, GIANT PLANET, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, methods: observational, OBJECT PROCESSING SYSTEM, Astrophysics - Earth and Planetary Astrophysics
Abstract

During the planet formation process, billions of comets are created and ejected into interstellar space. The detection and characterization of such interstellar comets (also known as extra-solar planetesimals or extra-solar comets) would give us in situ information about the efficiency and properties of planet formation throughout the galaxy. However, no interstellar comets have ever been detected, despite the fact that their hyperbolic orbits would make them readily identifiable as unrelated to the solar system. Moro-Mart\'in et al. 2009 have made a detailed and reasonable estimate of the properties of the interstellar comet population. We extend their estimates of detectability with a numerical model that allows us to consider "close" interstellar comets, e.g., those that come within the orbit of Jupiter. We include several constraints on a "detectable" object that allow for realistic estimates of the frequency of detections expected from the Large Synoptic Survey Telescope (LSST) and other surveys. The influence of several of the assumed model parameters on the frequency of detections is explored in detail. Based on the expectation from Moro-Mart\'in et al. 2009, we expect that LSST will detect 0.001-10 interstellar comets during its nominal 10-year lifetime, with most of the uncertainty from the unknown number density of small (nuclei of $\sim$0.1-1 km) interstellar comets. Using simulated LSST-like astrometric data, we study the problem of orbit determination for these bodies, finding that LSST could identify their orbits as hyperbolic and determine an ephemeris sufficiently accurate for follow-up in about 4-7 days. We give the hyperbolic orbital parameters of the most detectable interstellar comets. Taking the results into consideration, we give recommendations to future searches for interstellar comets., Comment: Published in Astrophysical Journal, 18 pages, 5 figures

Published
2016

15. Organic Matter in Cosmic Dust

Author

Scott A. Sandford, Alessandra Rotundi, Cécile Engrand, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM AS), and Université Paris-Saclay-Univ. Paris-Sud-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Solar System, STARDUST, AROMATIC-HYDROCARBONS, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Earth science, Comet dust, Astrophysics::Cosmology and Extragalactic Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, Article, Astrobiology, SOLAR-SYSTEM, Microanalysis, MOLECULES, Interplanetary dust cloud, Organics, Geochemistry and Petrology, ANTARCTIC MICROMETEORITES, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), PARTICLES, Organic matter, 010303 astronomy & astrophysics, Stratosphere, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, INTERPLANETARY DUST, chemistry.chemical_classification, [PHYS]Physics [physics], Carbonaceous matter, Hydrocarbons, ORIGIN, Extraterrestrial materials, C-H, chemistry, 13. Climate action, SNOW, Extraterrestrial life, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract

Organics are observed to be a significant component of cosmic dust in nearly all environments were dust is observed. In many cases only remote telescope observations of these materials are obtainable and our knowledge of the nature of these materials is very basic. However, it is possible to obtain actual samples of extraterrestrial dust in the Earth’s stratosphere, in Antarctic ice and snow, in near-Earth orbit, and via spacecraft missions to asteroids and comets. It is clear that cosmic dust contains a diverse population of organic materials that owe their origins to a variety of chemical processes occurring in many different environments. The presence of isotopic enrichments of D and 15N suggests that many of these organic materials have an interstellar/protosolar heritage. The study of these samples is of considerable importance since they are the best preserved materials of the early Solar System available.

Published
2016

16. Applications of Electrified Dust and Dust Devil Electrodynamics to Martian Atmospheric Electricity

Author

Jean-Jacques Berthelier, Nilton O. Renno, William M. Farrell, M. Zimmerman, Erika Barth, Francesca Esposito, Cauê S. Borlina, Franck Montmessin, Grégoire Déprez, Jonathan Merrison, Keri Nicoll, R. G. Harrison, Isobel M P Houghton, Karen Aplin, Sachchida Nand Tripathi, Department of Meteorology [Reading], University of Reading ( UOR ), Southwest Research Institute [Boulder] ( SwRI ), INAF - Osservatorio Astronomico di Capodimonte ( OAC ), Istituto Nazionale di Astrofisica ( INAF ), Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of Oxford [Oxford], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), University of Michigan [Ann Arbor], NASA Goddard Institute for Space Studies ( GISS ), NASA Goddard Space Flight Center ( GSFC ), Norwegian University of Science and Technology [Trondheim] ( NTNU ), Johns Hopkins University ( JHU ), UK’s Natural Environment Research Council (NE/L011514/1), University of Reading (UOR), Southwest Research Institute [Boulder] (SwRI), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan System-University of Michigan System, NASA Goddard Institute for Space Studies (GISS), NASA Goddard Space Flight Center (GSFC), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU), Johns Hopkins University (JHU), and University of Oxford

Subjects
[ SDU.OCEAN ] Sciences of the Universe [physics]/Ocean, Atmosphere, 010504 meteorology & atmospheric sciences, Particle electrification, OXIDANT ENHANCEMENT, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], WIND-BLOWN SAND, Atmospheric sciences, 01 natural sciences, GRANULAR INSULATOR SYSTEMS, SOLAR-SYSTEM, Atmosphere, Interplanetary dust cloud, Martian surface, 0103 physical sciences, 010303 astronomy & astrophysics, Dust devil, Lightning discharge, 0105 earth and related environmental sciences, Physics, Martian, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, FIELD METER, ION MEASUREMENTS, Global circuit, MARS, Hygroelectricity, Astronomy and Astrophysics, Atmosphere of Mars, ELECTROSTATIC DISCHARGES, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], PARTICLE-SIZE, 13. Climate action, Space and Planetary Science, CONTACT ELECTRIFICATION, Atmospheric electricity, Planetary electrostatics
Abstract

International audience; Atmospheric transport and suspension of dust frequently brings electrification, which may be substantial. Electric fields of 10 kV m−1 to 100 kV m−1 have been observed at the surface beneath suspended dust in the terrestrial atmosphere, and some electrification has been observed to persist in dust at levels to 5 km, as well as in volcanic plumes. The interaction between individual particles which causes the electrification is incompletely understood, and multiple processes are thought to be acting. A variation in particle charge with particle size, and the effect of gravitational separation explains to, some extent, the charge structures observed in terrestrial dust storms. More extensive flow-based modelling demonstrates that bulk electric fields in excess of 10 kV m−1 can be obtained rapidly (in less than 10 s) from rotating dust systems (dust devils) and that terrestrial breakdown fields can be obtained. Modelled profiles of electrical conductivity in the Martian atmosphere suggest the possibility of dust electrification, and dust devils have been suggested as a mechanism of charge separation able to maintain current flow between one region of the atmosphere and another, through a global circuit. Fundamental new understanding of Martian atmospheric electricity will result from the ExoMars mission, which carries the DREAMS (Dust characterization, Risk Assessment, and Environment Analyser on the Martian Surface)—MicroARES (Atmospheric Radiation and Electricity Sensor) instrumentation to Mars in 2016 for the first in situ electrical measurements.

Published
2016

17. Cometary Isotopic Measurements

Author

Dominique Bockelée-Morvan, A. Gicquel, Myrtha Hässig, Ursina Calmonte, Eva Wirström, J. Duprat, Simon Sheridan, Emmanuel Jehin, Bernard Marty, Philippe Rousselot, Steven B. Charnley, Stefanie N. Milam, Hideyo Kawakita, Cécile Engrand, Andrew Morse, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Space Research and Planetary Sciences [Bern) (WP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Astrochemistry Laboratory [Greenbelt], NASA Goddard Space Flight Center (GSFC), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Southwest Research Institute [San Antonio] (SwRI), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], This work was supported by NASA’s Planetary Astronomy and Planetary Atmospheres Programs (SNM and SBC), and by the Swedish Space Board (ESW)., Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM AS), and Université Paris-Saclay-Univ. Paris-Sud-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Solar System, Dark clouds, 010504 meteorology & atmospheric sciences, 530 Physics, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], INTERPLANETARY DUST PARTICLES, 01 natural sciences, Grain surface chemistry, Dense interstellar clouds, Astrobiology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Isotopes, ABUNDANCE RATIO, 0103 physical sciences, Comets, Astrophysics::Solar and Stellar Astrophysics, Low-Mass, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, O1 Hale-bopp, Physics, [PHYS]Physics [physics], Astronomy, Interplanatary dust particules, Astronomy and Astrophysics, GRAIN SURFACE-CHEMISTRY, C/1995 O1, Ultracarbonaceous antarctic micrometeorites, Space observatory, Planetary science, Deuterium, 13. Climate action, Space and Planetary Science, Abundance ratios, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Solar-system
Abstract

International audience; Isotopic ratios in comets provide keys for the understanding of the origin of cometary material, and the physical and chemical conditions in the early Solar Nebula. We review here measurements acquired on the D/H, N-14/N-15, O-16/O-18, C-12/C-13, and S-32/S-34 ratios in cometary grains and gases, and discuss their cosmogonic implications. The review includes analyses of potential cometary material available in collections on Earth, recent measurements achieved with the Herschel Space Observatory, large optical telescopes, and Rosetta, as well as recent results obtained from models of chemical-dynamical deuterium fractionation in the early solar nebula. Prospects for future measurements are presented.

Published
2015

18. 14N/15N ratio measurements in prestellar cores with N2H+: new evidence of 15N-antifractionation

Author

Jorma Harju, Luca Dore, E. Leonardo, Luca Bizzocchi, Elena Redaelli, Paola Caselli, Ana Chacón-Tanarro, Department of Physics, Redaelli, E., Bizzocchi, L., Caselli, P., Harju, J., Chacón-Tanarro, A., Leonardo, E., and Dore, L.

Subjects
Solar System, STARLESS CORES, 010504 meteorology & atmospheric sciences, NITROGEN ISOTOPIC FRACTIONATION, FOS: Physical sciences, DUST, ISM: molecule, Astrophysics, ISM: clouds, 01 natural sciences, ISM: abundances, GAS TEMPERATURE, SOLAR-SYSTEM, RADIATIVE-TRANSFER, ISM: cloud, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, radio lines: ISM, stars: formation, Molecular cloud, L694-2, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, ISM: abundance, ISM: molecules, HYPERFINE EXCITATION, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, DEPLETION
Abstract

Context: The $^{15}$N fractionation has been observed to show large variations among astrophysical sources, depending both on the type of target and on the molecular tracer used. These variations cannot be reproduced by the current chemical models. Aims: Until now, the $^{14}$N/$^{15}$N ratio in N$_2$H$^+$ has been accurately measured in only one prestellar source, L1544, where strong levels of fractionation, with depletion in $^{15}$N, are found ($^{14}$N/$^{15}$N$\: \approx 1000$). In this paper we extend the sample to three more bona fide prestellar cores, in order to understand if the antifractionation in N$_2$H$^+$ is a common feature of this kind of sources. Methods: We observed N$_2$H$^+$,N$^{15}$NH$^+$ and $^{15}$NNH$^+$ in L183, L429 and L694-2 with the IRAM 30m telescope. We modeled the emission with a non-local radiative transfer code in order to obtain accurate estimates of the molecular column densities, including the one for the optically thick N$_2$H$^+$. We used the most recent collisional rate coefficients available, and with these we also re-analysed the L1544 spectra previously published. Results: The obtained isotopic ratios are in the range $630-770$ and significantly differ with the value, predicted by the most recent chemical models, of $\approx 440$, close to the protosolar value. Our prestellar core sample shows high level of depletion of $^{15}$N in diazenylium, as previously found in L1544. A revision of the N chemical networks is needed in order to explain these results., Comment: Accepted for publication in A&A

Published
2018

19. ALMA Resolves C i Emission from the β Pictoris Debris Disk

Author

Aki Roberge, Inga Kamp, Göran Olofsson, Bernard L. de Vries, Alexis Brandeker, Gianni Cataldi, Yanqin Wu, René Liseau, William R. F. Dent, Eric Pantin, C. H. Chen, and Astronomy

Subjects
COLLISIONS, Planetesimal, Solar System, CIRCUMSTELLAR DISK, Astrophysics, Spatial distribution, circumstellar matter, 01 natural sciences, 010305 fluids & plasmas, SOLAR-SYSTEM, Tidal disruption event, Planet, GAS EMISSION, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, DESTRUCTION, Physics, Debris disk, Resonance, stars: individual (beta Pictoris), submillimeter: planetary systems, Astronomy and Astrophysics, HST-GHRS OBSERVATIONS, EVOLUTION, CO, radiative transfer, techniques: interferometric, Space and Planetary Science, PLANETESIMALS, Astrophysics::Earth and Planetary Astrophysics, methods: observational, NEARBY STARS, Astrophysics - Earth and Planetary Astrophysics
Abstract

The debris disk around $\beta$~Pictoris is known to contain gas. Previous ALMA observations revealed a CO belt at $\sim$85 au with a distinct clump, interpreted as a location of enhanced gas production. Photodissociation converts CO into C and O within $\sim$50 years. We resolve CI emission at 492 GHz using ALMA and study its spatial distribution. CI shows the same clump as seen for CO. This is surprising, as C is expected to quickly spread in azimuth. We derive a low C mass (between $5\times10^{-4}$ and $3.1\times10^{-3}$ M$_\oplus$), indicating that gas production started only recently (within $\sim$5000 years). No evidence is seen for an atomic accretion disk inwards of the CO belt, perhaps because the gas did not yet have time to spread radially. The fact that C and CO share the same asymmetry argues against a previously proposed scenario where the clump is due to an outward migrating planet trapping planetesimals in an resonance; nor can the observations be explained by an eccentric planetesimal belt secularly forced by a planet. Instead, we suggest that the dust and gas disks should be eccentric. Such a configuration, we further speculate, might be produced by a recent tidal disruption event. Assuming that the disrupted body has had a CO mass fraction of 10%, its total mass would be $\gtrsim$3 $M_\mathrm{Moon}$., Comment: 30 pages, 15 figures, accepted by ApJ

Published
2018

20. Review of Saturn’s icy moons following the Cassini mission

Author

Michele K. Dougherty and Linda Spilker

Subjects
LIQUID WATER, General Physics, 010504 meteorology & atmospheric sciences, Saturn (rocket family), Physics, Multidisciplinary, General Physics and Astronomy, Cassini-Huygens, 01 natural sciences, Astrobiology, SOLAR-SYSTEM, 0103 physical sciences, Instrumentation (computer programming), 010303 astronomy & astrophysics, 01 Mathematical Sciences, 0105 earth and related environmental sciences, Physics, SOUTH-POLAR TERRAIN, Science & Technology, 02 Physical Sciences, Spacecraft, IMAGING SCIENCE, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Icy moon, SMALL SATELLITES, WATER RESERVOIR, PLUME, Saturn, Physical Sciences, Physics::Space Physics, E-RING, ENCELADUS, IAPETUS, icy satellites, Astrophysics::Earth and Planetary Astrophysics, business
Abstract

We review our knowledge of the icy moons of Saturn prior to the Cassini orbital mission, describe the discoveries made by the instrumentation onboard the Cassini spacecraft.

Published
2018

21. OSIRIS – The Scientific Camera System Onboard Rosetta

Author

Marco Fulle, K.-P. Wenzel, Fritz Gliem, A. López, Jean-Pierre Sivan, Rafael Rodrigo, Detlef Koschny, U. Telljohann, Nicolas Thomas, G. Parzianello, Kjetil Dohlen, R. Muller, K. Stöckner, Michael Küppers, Gian Paolo Guizzo, Giampiero Naletto, J. J. López-Moreno, Werner Curdt, J.-R. Kramm, V. Timon, Mirco Zaccariotto, D. Germerott, P. Ramous, Francesco Angrilli, Joseph A. Burns, M. Angulo, K.-U. Reiche, M. D. Michelena, Sonia Fornasier, T. Wittrock, M. Reina, Marco Pertile, H. U. Keller, Michael F. A'Hearn, A. Sanz, C. Quintana, Luisa Lara, A. Llebaria, Wing-Huen Ip, Laurent Jorda, L. Sabau, Peter Barthol, M. E. Bailey, Harald Michalik, Gérard Rousset, Stubbe F. Hviid, I. Büttner, José María Bermúdez de Castro, Hans Rickman, Gabriele Cremonese, Alain Origne, Holger Sierks, Stefano Debei, Roberto Ragazzoni, M. De Cecco, A. Lopez-Jimenez, Jean-Loup Bertaux, Cesare Barbieri, V. Brown, M. A. Barucci, J.-L. Boit, J. E. Rodriguez, Philippe Lamy, R. Meller, G. Bianchini, V. Da Deppo, J. Tabero, Ekkehard Kührt, G. Tomasch, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Space Physics [Uppsala], Uppsala University, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Instituto Nacional de Técnica Aeroespacial (INTA), Armagh Observatory [Armagh], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), Institut für Datentechnik und Kommunikationsnetze, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Carlo Gavazzi Space SpA (CGS), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Universidad Politécnica de Madrid (UPM), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Agence Spatiale Européenne = European Space Agency (ESA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung (MPS), Universita degli Studi di Padova, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Space Agency (ESA)-European Space Agency (ESA), Consiglio Nazionale delle Ricerche [Roma] (CNR), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Cornell University, and Technische Universität Braunschweig [Braunschweig]

Subjects
010504 meteorology & atmospheric sciences, Comet, Cometary activity, Coma (optics), Spectroscopic, Osiris, 7. Clean energy, 01 natural sciences, Aeronáutica, Data processing system, SOLAR-SYSTEM, Imaging system, comet, WIDE-ANGLE CAMERA, Shutter, Rosetta, 0103 physical sciences, SOUTHERN SPECTROPHOTOMETRIC STANDARDS, Angular resolution, Wide angle camera, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Physics, camera system, Spacecraft, biology, business.industry, Detector, Astronomy, Astronomy and Astrophysics, biology.organism_classification, COMET HALLEY, Narrow angle camera, Space and Planetary Science, DUST JETS, Camera, business
Abstract

The Optical, Spectroscopic, and Infrared Remote Imaging System OSIRIS is the scientific camera system onboard the Rosetta spacecraft (Figure 1). The advanced high performance imaging system will be pivotal for the success of the Rosetta mission. OSIRIS will detect 67P/Churyumov-Gerasimenko from a distance of more than 106 km, characterise the comet shape and volume, its rotational state and find a suitable landing spot for Philae, the Rosetta lander. OSIRIS will observe the nucleus, its activity and surroundings down to a scale of ~2 cm px−1. The observations will begin well before the onset of cometary activity and will extend over months until the comet reaches perihelion. During the rendezvous episode of the Rosetta mission, OSIRIS will provide key information about the nature of cometary nuclei and reveal the physics of cometary activity that leads to the gas and dust coma. OSIRIS comprises a high resolution Narrow Angle Camera (NAC) unit and a Wide Angle Camera (WAC) unit accompanied by three electronics boxes. The NAC is designed to obtain high resolution images of the surface of comet 67P/Churyumov-Gerasimenko through 12 discrete filters over the wavelength range 250–1000 nm at an angular resolution of 18.6 μrad px−1. The WAC is optimised to provide images of the near-nucleus environment in 14 discrete filters at an angular resolution of 101 μrad px−1. The two units use identical shutter, filter wheel, front door, and detector systems. They are operated by a common Data Processing Unit. The OSIRIS instrument has a total mass of 35 kg and is provided by institutes from six European countries. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Sweden (SNSB), and Spain (MEC) is gratefully acknowledged. Substantial support for the development of the Data Processing Unit was provided by the ESA Technical Directorate through the Technical Research Programme. In addition to the formal co-authors of this paper (comprising lead scientists, Co-Is, project managers, and lead engineers ), the project was supported by an enormous number of scientists, engineers, and technicians involved in the day-to-day development of the hardware. These include J. C. Blanc, D. Pouliquen, M. Saisse (France), A. Alvarez, A. L. Arteaga, A. Carretero, M. Fernández, H. Guerrero, P. Gutiérrez, J. L. Lizondo, V. Luengo, J. A. Martín, M. A. Martín, J. Meseguer, J. M. Mi, L. Moreno, J. Navarro, A. Núñez, E. Ragel, D. Rodríguez, G. Rosa, A. Sanchez, J. C. Sanmartín, G. Tonellotto (Spain), W. Boogaerts, W. Engelhardt, K. Eulig, B. Fiethe, A. Fischer, M. Gartner, K. Grabig, K. Kellner, A. Kiihn. W. Kiihn. J. Knollenberg, W. Neumann, J. Nitsch, P. Rüffer, H. Schüddekopf, U. Schiihlc. I. Sebastian, S. Stelzer, U. Strohmeyer, T. Tzscheetzsch, M. Wassermeyer (Germany), B. Johlander (ESTEC), M. Baessato, P. F. Brunello, S. Casotto, F. Don-, M. Lazzarin, E. Marchetti, F. Marzari, P. G. Nicolosi, F. Perón, F. Rampazzi, B. Saggin, G. Tondello, S. Verani, P. Zambolin ' (Italy), J. Lagerros, and B. Davidsson (Sweden). Peerreview

Published
2007

22. Planck 2013 results. XIV. Zodiacal emission

Author

Olivier Forni, M.-A. Miville-Deschênes, Reijo Keskitalo, F. K. Hansen, M. Ashdown, L. Montier, H. K. Eriksen, Douglas J. Marshall, J.-P. Bernard, Benjamin D. Wandelt, Julian Borrill, Jérôme Bobin, Davide Maino, A. Chamballu, Jean-Luc Starck, F. Cuttaia, E. Franceschi, James J. Bock, S. Mottet, J. F. Macías-Pérez, Clive Dickinson, K. Ganga, Anna Bonaldi, W. Hovest, E. Martínez-González, M. Piat, Anne Lähteenmäki, A. Curto, T. Poutanen, Jose M. Diego, S. Galeotta, C. Hernández-Monteagudo, Charles R. Lawrence, Alessandro Gruppuso, J. A. Murphy, Graca Rocha, Kevin M. Huffenberger, Pasquale Mazzotta, M. Tucci, Roberta Paladini, R. Stompor, R. B. Barreiro, Marian Douspis, M. Sandri, F. Piacentini, Xun Chen, François R. Bouchet, O. Perdereau, M. Rowan-Robinson, Peter Meinhold, P. B. Lilje, J.-M. Lamarre, George Helou, D. Yvon, Olivier Doré, J. González-Nuevo, Silvia Masi, Alessandro Melchiorri, Fabrizio Villa, Jacques Delabrouille, Hannu Kurki-Suonio, M. Tomasi, George F. Smoot, Ben Rusholme, Andrea Zacchei, B. Van Tent, Theodore Kisner, L. Toffolatti, René J. Laureijs, M. Frailis, Carlo Baccigalupi, C. Armitage-Caplan, S. Osborne, Fabio Finelli, A. J. Banday, D. Tavagnacco, E. Hivon, James G. Bartlett, Lloyd Knox, A. Coulais, L. Perotto, David L. Clements, J. Lesgourgues, Anthony Lasenby, Jussi-Pekka Väliviita, G. Patanchon, F. Couchot, W. C. Jones, J.-F. Sygnet, F. Paci, A. M. Polegre, M. Maris, Rafael Rebolo, Bruno Maffei, L. P. L. Colombo, S. Donzelli, G. Roudier, F. Pasian, Marco Bersanelli, Dmitry Novikov, F. Pajot, Luca Valenziano, G. W. Pratt, E. Pierpaoli, L. A. Wade, E. Keihänen, Daniela Paoletti, D. Herranz, Gianluca Morgante, G. de Zotti, R. Sudiwala, Andrea Zonca, A. Gregorio, Dipak Munshi, George Efstathiou, A. A. Fraisse, N. Mandolesi, R. C. Butler, H. C. Chiang, D. Sutton, Andrew H. Jaffe, G. Umana, J. Tuovinen, Philip Lubin, F. Atrio-Barandela, S. Ricciardi, P. de Bernardis, Alain Benoit, Giorgio Savini, Torsten A. Enßlin, W. A. Holmes, William T. Reach, C. Rosset, S. Colombi, Stéphane Plaszczynski, T. Riller, R. D. Davies, A. Catalano, M. Tristram, P. Vielva, Ranga-Ram Chary, Jörg P. Rachen, D. L. Harrison, G. Polenta, M. Linden-Vørnle, Sarah E. Church, J. Aumont, Luigi Danese, Serge Gratton, X. Dupac, Pavel Naselsky, T. R. Jaffe, F.-X. Désert, A. Benoit-Lévy, J.-M. Delouis, Michele Liguori, M. Giard, M. Migliaccio, R. Kneissl, L. Popa, E. P. S. Shellard, Marcella Massardi, Guilaine Lagache, L. Mendes, B. P. Crill, N. Ponthieu, A.-S. Suur-Uski, Lung-Yih Chiang, A. Mennella, Nabila Aghanim, Sabino Matarrese, F. Perrotta, K. Benabed, Nicola Vittorio, Peter A. R. Ade, Créidhe O'Sullivan, M. López-Caniego, Michael Seiffert, Florent Sureau, J. R. Bond, Duncan Hanson, Michael P. Hobson, Jean-François Cardoso, F. Boulanger, R. Leonardi, J.-M. Colley, Daniel J. Mortlock, H. Dole, Subhabrata Mitra, J. A. Tauber, I. D. Novikov, J.-L. Puget, G. Prézeau, D. Santos, Allan Hornstrup, Etienne Pointecouteau, S. R. Hildebrandt, Carlo Burigana, Krzysztof M. Gorski, P. R. Christensen, F. Matthai, M. Bucher, Douglas Scott, Mika Juvela, Davide Pietrobon, F. Noviello, Calvin B. Netterfield, A. Moneti, Y. Giraud-Héraud, I. Ristorcelli, Monique Arnaud, Federico Nati, Luca Terenzi, Hans Ulrik Nørgaard-Nielsen, M. Bridges, C. Renault, J. Knoche, Simon Prunet, P. Bielewicz, Sophie Henrot-Versille, Paolo Natoli, M. Reinecke, C. A. Oxborrow, A. de Rosa, Peter G. Martin, Locke D. Spencer, E. Battaner, V. Stolyarov, Martin Kunz, Mathieu Remazeilles, L. Pagano, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], Tauber, J, Ade, P, Aghanim, N, Armitage Caplan, C, Arnaud, M, Ashdown, M, Atrio Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartlett, J, Battaner, E, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, J, Bonaldi, A, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bridges, M, Bucher, M, Burigana, C, Butler, R, Cardoso, J, Catalano, A, Chamballu, A, Chary, R, Chen, X, Chiang, H, Chiang, L, Christensen, P, Church, S, Clements, D, Colley, J, Colombi, S, Colombo, L, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, J, Désert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, T, Eriksen, H, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giraud Héraud, Y, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hanson, D, Harrison, D, Helou, G, Henrot Versillé, S, Hernández Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Laureijs, R, Lawrence, C, Leonardi, R, Lesgourgues, J, Liguori, M, Lilje, P, Linden Vørnle, M, López Caniego, M, Lubin, P, MacIás Pérez, J, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martínez González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville Deschênes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Mottet, S, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nørgaard Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, O'Sullivan, C, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polegre, A, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rowan Robinson, M, Rusholme, B, Sandri, M, Santos, D, Savini, G, Scott, D, Seiffert, M, Shellard, E, Smoot, G, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sureau, F, Sutton, D, Suur Uski, A, Sygnet, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, Yvon, D, Zacchei, A, Zonca, A, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Tauber, Jan, Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Chamballu, A., Chary, R. R., Chen, X., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colley, J. M., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., MacIás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Mottet, S., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., O'Sullivan, C., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polegre, A. M., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan Robinson, M., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Smoot, G. F., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., Zonca, A., Department of Physics, Helsinki Institute of Physics, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Universidad de Cantabria

Subjects
Solar System, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, IRAS OBSERVATIONS, Cosmic microwave background, COBE, Astrophysics, cosmic background radiation, Cosmic background radiation, 7. Clean energy, 01 natural sciences, Interplanetary medium, Zodiacal dust, Interplanetary dust cloud, 010303 astronomy & astrophysics, media_common, Physics, PLANCK MISSION, SYSTEM DUST BANDS, ORIGIN, Astrophysics::Instrumentation and Methods for Astrophysics, Celestial sphere, Computer Science::Computers and Society, Wavelength, Physics::Space Physics, Physical Sciences, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, symbols, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, interplanetary medium, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, INFRARED-EMISSION, COMETARY, Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, NO, SOLAR-SYSTEM, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, interplanetar medium, 0103 physical sciences, Planck, Astrophysics::Galaxy Astrophysics, Astronomy and Astrophysics, Space and Planetary Science, SPECTRUM, Zodiacal light, Science & Technology, 010308 nuclear & particles physics, zodiacal dust, Astronomy and Astrophysic, 115 Astronomy, Space science, CLOUD, MODEL, 0201 Astronomical And Space Sciences, 13. Climate action, Sky
Abstract

The Planck satellite provides a set of all-sky maps at nine frequencies from 30GHz to 857GHz. Planets, minor bodies, and diffuse interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through different columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model-a diffuse cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

Published
2014

23. NIR spectral trends of HED meteorites: Can we discriminate between the magmatic evolution, mechanical mixing and observation geometry effects?

Author

Frédéric Moynier, Eric Quirico, Pierre Beck, Bernard Schmitt, Jean-Alix Barrat, Christian Beck, F. Grisolle, Philippe Gillet, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Domaines Océaniques (LDO), Centre National de la Recherche Scientifique (CNRS)-Institut d'écologie et environnement-Observatoire des Sciences de l'Univers-Université de Brest (UBO)-Institut national des sciences de l'Univers (INSU - CNRS), McDonnell Center for Space Sciences, Washington University in St Louis, Department of Earth and Planetary Sciences [St Louis], Institut de Physique de la Matière Condensée (EPFL), Ecole Polytechnique Fédérale de Lausanne (EPFL), Mécanique des failles, Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF), CNES, the Programme National de Planétologie, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Observatoire des Sciences de l'Univers-Institut d'écologie et environnement-Centre National de la Recherche Scientifique (CNRS), Washington University in Saint Louis (WUSTL), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Materials science, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Iron, Howardite, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Nwa 2737, Geometry, Pyroxene, 01 natural sciences, Spectral line, Bidirectional Reflectance, 0103 physical sciences, Pyroxene Mixtures, Asteroid Vesta, 010303 astronomy & astrophysics, Asteroids, Composition, Planetary Surfaces, 0105 earth and related environmental sciences, Eucrite, Diogenite, Infrared observations, Diogenites, Near-infrared spectroscopy, Astronomy and Astrophysics, Eucrite Parent Body, Mineralogy, Asteroids, Geochemistry, Meteorite, 13. Climate action, Space and Planetary Science, Asteroid, Asteroid 4 Vesta, Solar-System, Composition, Meteorites, [SDU.STU.MI]Sciences of the Universe [physics]/Earth Sciences/Mineralogy
Abstract

The Howardite-Eucrite-Diogenite (HED) suite is a family of differentiated meteorites that provide a unique opportunity to study the differentiation of small bodies. The likely parent-body of this meteorite group, (4) Vesta is presently under study by the Dawn mission, scrutinizing its surface in the visible and NIR infrared range. Here, we discuss how well the magmatic trends observed in HED might be retrieved from NIR spectroscopy, by studying laboratory spectra of 10 HED meteorites together with spectra from the RELAB database. We show that although an exsolution process did occur for most eucrites (i.e. decomposition of a primary calcic pyroxene into a high-Ca and low-Ca pyroxene), it does not affect the "bulk pyroxene" trend retrieved from the location of the pyroxene crystal field bands (Band I with a maximum of absorption around at about 1 mu m and Band II around 2 mu m). Absolute values of the chemical composition appears however to deviate from the expected chemical composition. We show that mechanical mixture (i.e. impact gardening) will produce a linear mixing in the pyroxenes band position diagram (Band I position vs Band II position). This diagram also reveals that howardite are not pure mixtures of an average eucrite and average diogenite. Because asteroid surfaces are expected to show topography, we also study the effect of observation geometry on the NIR spectra of an eucrite and a diogenite by measuring the bi-directional reflectance spectra from 0.4 to 4.6 mu m. Results show that these meteorites tend to act as forward scatterers, leading to a decrease of integrated band area (relative to the continuum) at high phase angles. The position of the two strong crystal field bands shows only small variability with observation geometry. Retrieval of the magmatic trends from the Band I vs Band II diagram should not be affected by observation geometry effects. Finally we performed NIR reflectance measurement on olivine diogenites. The presence of olivine can be suggested by using the Band Area Ratio vs Band I diagram, but this phase might affect the retrieval of pyroxene composition from the position of Band I and Band II. (C) 2011 Elsevier Inc. All rights reserved.

Published
2011

24. Nature of volatile depletion and genetic relationships in enstatite chondrites and aubrites inferred from Zn isotopes

Author

Frédéric Moynier, Frank A. Podosek, Francis Albarède, Matthieu Gounelle, Randal C. Paniello, Brigitte Zanda, Pierre Beck, Department of Geology [Davis], University of California [Davis] (UC Davis), University of California-University of California, Department of Earth and Planetary Sciences [St Louis], Washington University in Saint Louis (WUSTL), McDonnell Center for Space Sciences, Laboratoire de Minéralogie et Cosmochimie du Muséum (LMCM), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Programme National de Planetologie (INSU-CEA), ANR, NASA, University of California (UC)-University of California (UC), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Geochemistry, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Isotopes of oxygen, Parent body, SOLAR-SYSTEM, ZINC, Geochemistry and Petrology, Chondrite, Breccia, TRACE-ELEMENTS, Achondrite, 0105 earth and related environmental sciences, ORIGIN, FRACTIONATION, THERMAL METAMORPHISM, Chondrule, LUNAR-SAMPLES, Meteorite, 13. Climate action, PRIMITIVE METEORITES, Enstatite, engineering, PARENT-BODY, IRON-METEORITES, Geology
Abstract

International audience; Enstatite meteorites include the undifferentiated enstatite chondrites and the differentiated enstatite achondrites (aubrites). They are the most reduced group of all meteorites. The oxygen isotope compositions of both enstatite chondrites and aubrites plot along the terrestrial mass fractionation line, which suggests some genetic links between these meteorites and the Earth as well. For this study, we measured the Zn isotopic composition of 25 samples from the following groups: aubrites (main group and Shallowater), EL chondrites, EH chondrites and Happy Canyon (impact-melt breccia). We also analyzed the Zn isotopic composition and elemental abundance in separated phases (metal, silicates, and sulfides) of the EH4, EL3, and EL6 chondrites. The different groups of meteorites are isotopically distinct and give the following values (parts per thousand): aubrite main group (-7.08 < delta Zn-66

Published
2011

25. Integrity and Biological Activity of DNA after UV Exposure

Author

Sébastien Dupraz, Jean-Michel Monier, Caroline Freissinet, Delina Lyon, Timothy M. Vogel, Pascal Simonet, Ampère (AMPERE), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Institut de Physique du Globe de Paris, Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, and Institut de Physique du Globe de Paris (IPG Paris)

Subjects
Ultraviolet Rays, Biology, Molecular cloning, 01 natural sciences, Polymerase Chain Reaction, GENE-TRANSFER, TRANSPLASTOMIC TOBACCO, UV radiation, law.invention, SOLAR-SYSTEM, 03 medical and health sciences, chemistry.chemical_compound, NATURAL TRANSFORMATION, Plasmid, Transformation, Genetic, law, PLASMID DNA, NUCLEIC-ACID, 0103 physical sciences, Ultramafic, ANCIENT DNA, CLAY-MINERALS, Extraterrestrial life, Biosignature, 010303 astronomy & astrophysics, Gene, Polymerase chain reaction, 0303 health sciences, EARTH ORBIT, 030306 microbiology, Oligonucleotide, DNA, Agricultural and Biological Sciences (miscellaneous), Molecular biology, Real-time polymerase chain reaction, chemistry, Space and Planetary Science, Nucleic acid, Clay, ACINETOBACTER SP, Aluminum Silicates, [SDE.BE]Environmental Sciences/Biodiversity and Ecology
Abstract

International audience; The field of astrobiology lacks a universal marker with which to indicate the presence of life. This study supports the proposal to use nucleic acids, specifically DNA, as a signature of life (biosignature). In addition to its specificity to living organisms, DNA is a functional molecule that can confer new activities and characteristics to other organisms, following the molecular biology dogma, that is, DNA is transcribed to RNA, which is translated into proteins. Previous criticisms of the use of DNA as a biosignature have asserted that DNA molecules would be destroyed by UV radiation in space. To address this concern, DNA in plasmid form was deposited onto different surfaces and exposed to UVC radiation. The surviving DNA was quantified via the quantitative polymerase chain reaction (qPCR). Results demonstrate increased survivability of DNA attached to surfaces versus non-adsorbed DNA. The DNA was also tested for biological activity via transformation into the bacterium Acinetobacter sp. and assaying for antibiotic resistance conferred by genes encoded by the plasmid. The success of these methods to detect DNA and its gene products after UV exposure (254 nm, 3.5 J/m(2)s) not only supports the use of the DNA molecule as a biosignature on mineral surfaces but also demonstrates that the DNA retained biological activity.

Published
2010

26. Cosmic spherules from Widerøefjellet, Sør Rondane Mountains (East Antarctica)

Author

Ian A. Franchi, Steven Goderis, Frank Vanhaecke, Vinciane Debaille, Flore Van Maldeghem, Stijn Van Malderen, Bastien Soens, Dan Topa, Matthias Van Ginneken, Philippe Claeys, Richard C. Greenwood, M. S. Huber, Christian Koeberl, Veerle Cnudde, Seann McKibbin, Hydrogeology, Environmental hydrogeology, Chemistry, Analytical, Environmental & Geo-Chemistry, Faculty of Sciences and Bioengineering Sciences, and Earth System Sciences

Subjects
010504 meteorology & atmospheric sciences, DRONNING MAUD LAND, DEEP-SEA SEDIMENTS, Geochemistry, INTERPLANETARY DUST PARTICLES, heating, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Oxygen isotope ratios, Isotopes of oxygen, Petrography, ACCRETION RATE, SOLAR-SYSTEM, Extraterrestrial dust, Chondrite, Geochemistry and Petrology, 0105 earth and related environmental sciences, OXYGEN ISOTOPIC COMPOSITIONS, PLATINUM-GROUP NUGGETS, Olivine, Parent bodies, Trace element, Géochimie, Pétrologie, TRACE-ELEMENT, Cosmic spherules, Chemistry, MOUNTAINS, Meteorite, 13. Climate action, Micrometeorite, Earth and Environmental Sciences, VICTORIA LAND, engineering, Sedimentary rock, TRANSANTARCTIC, Atmospheric heating, Atmospheric
Abstract

A newly discovered sedimentary accumulation of micrometeorites in the Sør Rondane Mountains of East Antarctica, close to the Widerøefjellet summit at ∼2750 m above sea level, is characterized in this work. The focus here lies on 2099 melted cosmic spherules larger than 200 μm, extracted from 3.2 kg of sampled sediment. Although the Widerøefjellet deposit shares similarities to the micrometeorite traps encountered in the Transantarctic Mountains, both subtle and more distinct differences in the physicochemical properties of the retrieved extraterrestrial particles and sedimentary host deposits are discernable (e.g. types of bedrock, degree of wind exposure, abundance of metal-rich particles). Unlike the Frontier Mountain and Miller Butte sedimentary traps, the size fraction below 240 μm indicates some degree of sorting at Widerøefjellet, potentially through the redistribution by wind, preferential alteration of smaller particles, or processing biases. However, the cosmic spherules larger than 300 μm appear largely unbiased following their size distribution, frequency by textural type, and bulk chemical compositions. Based on the available bedrock exposure ages for the Sør Rondane Mountains, extraterrestrial dust is estimated to have accumulated over a time span of ∼1–3 Ma at Widerøefjellet. Consequently, the Widerøefjellet collection reflects a substantial reservoir to sample the micrometeorite influx over this time interval. Petrographic observations and 3D microscopic CT imaging are combined with chemical and triple-oxygen isotopic analyses of silicate-rich cosmic spherules larger than 325 μm. The major element composition of 49 cosmic spherules confirms their principally chondritic parentage. For 18 glassy, 15 barred olivine, and 11 cryptocrystalline cosmic spherules, trace element concentrations are also reported on. Based on comparison with evaporation experiments reported in literature and accounting for siderophile and chalcophile element losses during high-density phase segregation and ejection, the observed compositional sequence largely reflects progressive heating and evaporation during atmospheric passage accompanied by significant redox shifts, although the influence of (refractory) chondrite mineral constituents and terrestrial alteration cannot be excluded in all cases. Twenty-eight cosmic spherules larger than 325 μm analyzed for triple-oxygen isotope ratios confirm inheritance from mostly carbonaceous chondritic precursor materials (∼55% of the particles). Yet, ∼30% of the measured cosmic spherules and ∼50% of all glassy cosmic spherules are characterized by oxygen isotope ratios above the terrestrial fractionation line, implying genetic links to ordinary chondrites and parent bodies currently unsampled by meteorites. The structural, textural, chemical, and isotopic characteristics of the cosmic spherules from the Sør Rondane Mountains, and particularly the high proportion of Mg-rich glass particles contained therein, imply a well-preserved and representative new sedimentary micrometeorite collection from a previously unstudied region in East Antarctica characterized by distinct geological and exposure histories., SCOPUS: ar.j, info:eu-repo/semantics/published

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