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

Maria Nikolayevna Drozdovskaya, Ewine F. van Dishoeck, Martin Rubin, Jes Kristian Jørgensen, Kathrin Altwegg
(Submitted on 8 Feb 2018)

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. Comments:    To appear in “Astrochemistry VII — Through the Cosmos from Galaxies to Planets”, proceedings of the IAU Symposium No. 332, 2017, Puerto Varas, Chile. M. Cunningham, T. Millar and Y. Aikawa, eds. (6 pages)
Subjects:    Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP)
Cite as:    arXiv:1802.02967 [astro-ph.SR] (or arXiv:1802.02967v1 [astro-ph.SR] for this version)
Submission history
From: Maria Drozdovskaya 
[v1] Thu, 8 Feb 2018 17:08:46 GMT (21kb)
https://arxiv.org/abs/1802.02967
Astrochemistry