Cometary Isotopic Measurements

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 cometa...

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Bibliographic Details
Published in:Space Science Reviews
Main Authors: Bockelee-Morvan, D, Calmonte, U, Charnley, S, Duprat, J, Engrand, C, Gicquel, A, Haessig, M, Jehin, E, Kawakita, H, Marty, B, Milam, S, Morse, A, Rousselot, P, Sheridan, S, Wirstrom, E
Other Authors: 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), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM AS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Univ. Paris-Sud
Format: Article in Journal/Newspaper
Language:English
Published: HAL CCSD 2015
Subjects:
Online Access:http://hal.in2p3.fr/in2p3-01251164
https://doi.org/10.1007/s11214-015-0156-9
Description
Summary: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.