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ALMA observations of sulfur-bearing molecules in protoplanetary disks

Published online by Cambridge University Press:  13 January 2020

H. Nomura ,
A. Higuchi ,
N. Sakai ,
S. Yamamoto ,
M. Nagasawa ,
K.K. Tanaka ,
H. Miura ,
T. Nakamoto ,
H. Tanaka  and
T. Yamamoto
...Show all authors
H. Nomura
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Japan
A. Higuchi
Affiliation:
RIKEN Cluster for Pioneering Research, Japan
N. Sakai
Affiliation:
RIKEN Cluster for Pioneering Research, Japan
S. Yamamoto
Affiliation:
Department of Physics, The University of Tokyo, Japan
M. Nagasawa
Affiliation:
School of Medicine, Kurume University, Japan
K.K. Tanaka
Affiliation:
Department of Astronomy, Tohoku University, Japan
H. Miura
Affiliation:
Graduate School of Natural Sciences, Nagoya City University, Japan
T. Nakamoto
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Japan
H. Tanaka
Affiliation:
Department of Astronomy, Tohoku University, Japan
T. Yamamoto
Affiliation:
Institute of Low Temperature Science, Hokkaido University, Japan
C. Walsh
Affiliation:
School of Physics and Astronomy, University of Leeds, UK
T.J. Millar
Affiliation:
ARC, School of Mathematics and Physics, Queen’s University Belfast, UK Leiden Observatory, Leiden University, The Netherlands
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Abstract

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It is thought that protoplanets formed in protoplanetary disks excite the orbital motion of the surrounding planetesimals, and the bow shocks caused by the highly excited planetesimals heat their icy component evaporating into gas. We have performed model calculations to study the evolution of molecular abundances of the evaporated icy component, which suggests sulfur-bearing molecules can be good tracers of icy planetesimal evaporation. Here we report the result of our ALMA observations of sulfur-bearing molecules towards protoplanetary disks. The lines were undetected but the obtained upper limits of the line fluxes and our model calculations give upper limits of the fractional abundances of x(H2S) < 10−11 and x(SO) < 10−10 in the outer disk. These results are consistent with the molecular abundances in comets in our Solar system.

Keywords

astrochemistryplanetary systems: protoplanetary disksISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 360 - 361
Copyright
© International Astronomical Union 2020 

References

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