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The chemical connection between 67P/C-G and IRAS 16293-2422

Published online by Cambridge University Press:  04 September 2018

Maria Nikolayevna Drozdovskaya Open the ORCID record for Maria Nikolayevna Drozdovskaya [Opens in a new window] ,
Ewine F. van Dishoeck ,
Martin Rubin ,
Jes Kristian Jørgensen  and
Kathrin Altwegg Open the ORCID record for Kathrin Altwegg [Opens in a new window]
Maria Nikolayevna Drozdovskaya
Affiliation:
Center for Space and Habitability (CSH), Universität Bern Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected]
Ewine F. van Dishoeck
Affiliation:
Leiden Observatory, Leiden UniversityPO Box 9513, NL-2300 RA Leiden, The Netherlands email: [email protected] Max-Planck Institut für Extraterrestrische Physik (MPE) Giessenbachstrasse 1, 85748 Garching, Germany
Martin Rubin
Affiliation:
Physikalisches Institut, Universität Bern Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected]
Jes Kristian Jørgensen
Affiliation:
Centre for Star and Planet Formation Niels Bohr Institute & Natural History Museum of Denmark, University of Copenhagen Øster Voldgade 57, DK-1350 Copenhagen K., Denmark email: [email protected]
Kathrin Altwegg
Affiliation:
Center for Space and Habitability (CSH), Universität Bern Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected] Physikalisches Institut, Universität Bern Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected] email: [email protected]
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Abstract

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The chemical evolution of a star- and planet-forming system begins in the prestellar phase and proceeds across the subsequent evolutionary phases. The chemical trail from cores to protoplanetary disks to planetary embryos can be studied by comparing distant young protostars and comets in our Solar System. One particularly chemically rich system that is thought to be analogous to our own is the low-mass IRAS 16293-2422. ALMA-PILS observations have made the study of chemistry on the disk scales (<100 AU) of this system possible. Under the assumption that comets are pristine tracers of the outer parts of the innate protosolar disk, it is possible to compare the composition of our infant Solar System to that of IRAS 16293-2422. The Rosetta mission has yielded a wealth of unique in situ measurements on comet 67P/C-G, making it the best probe to date. Herein, the initial comparisons in terms of the chemical composition and isotopic ratios are summarized. Much work is still to be carried out in the future as the analysis of both of these data sets is still ongoing.

Keywords

astrochemistrycomets: individual (67P/C-G)stars: individual (IRAS 16293-2422)(stars:) planetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 196 - 201
Copyright
Copyright © International Astronomical Union 2018 

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