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Chemical Change in the Disk Forming Region of IRAS 16293–2422 Studied with ALMA

Published online by Cambridge University Press:  04 September 2018

Yoko Oya Open the ORCID record for Yoko Oya [Opens in a new window]
Yoko Oya*
Affiliation:
Department of Physics, The University of Tokyo, Bunkyo-ku, Tokyo, 113-0033, Japan email: oya@taurus.phys.s.u-tokyo.ac.jp
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Abstract

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We have analyzed rotational spectral line emission of OCS, CH3OH, HCOOCH3, and H2CS observed toward the low-mass Class 0 protostar IRAS 16293–2422 (Source A and B) at a sub-arcsecond resolution with ALMA. Significant chemical differentiation is found at a 50 au scale. OCS is found to trace the infalling-rotating envelope, while COM distributions are concentrated around the inner part of the envelope. The kinematic structure in Source A is explained with a ballistic model, and the protostellar mass and the radius of the centrifugal barrier are evaluated to be ~0.75 M⊙ and ~50 au, respectively. This study has revealed that the centrifugal barrier plays a central role not only in the disk formation but also in the associated chemical evolution.

Keywords

ALMAIRAS 16293–2422MoleculesDisk formation
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. 73 - 80
Copyright
Copyright © International Astronomical Union 2018 

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