2017/09/27 by Liton Majumdar, J-C Loison, Jean-Christophe Loison +6 · 31 citations
Chemistry · Physics and Astronomy · #Advanced Chemical Physics Studies #Astrobiology #Astrophysics #Astrophysics and Star Formation Studies #Comet #Molecular Spectroscopy and Structure #Phase (matter) #Physics #Protostar #Solar System #Star formation #Stars #astro-ph.GA
paper · pdf · doi:10.1093/mnrasl/slx157
published in Monthly Notices of the Royal Astronomical Society Letters 473(1), L59-L63 (Oxford University Press) · Accepted for publication in MNRAS Letters
openalex publication_date 2017/09/27 · arxiv created 2017/09/28 · arxiv updated 2017/12/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Methyl isocyanate (CH3NCO) is one of the important complex organic molecules detected on the comet 67P/Churyumov–Gerasimenko by Rosetta’s Philae lander. It was also detected in hot cores around high-mass protostars along with a recent detection in the solar-type protostar IRAS 16293−2422. We propose here a gas-grain chemical model to form CH3NCO after reviewing various formation pathways with quantum chemical computations. We have used nautilus three-phase gas-grain chemical model to compare observed abundances in the IRAS 16293−2422. Our chemical model clearly indicates the ice phase origin of CH3NCO.