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Evaporation of grain-surface species by shock waves onto a forming protoplanetary disk

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Yuri Aikawa ,
Takuhiro Aota  and
Tsuyoshi Inoue
Yuri Aikawa
Affiliation:
Center for Computer Sciences, University of Tsukuba email: aikawa@ccs.tsukuba.ac.jp
Takuhiro Aota
Affiliation:
Fuji Soft
Tsuyoshi Inoue
Affiliation:
Division of Theoretical Astronomy, National Astronomical Observatory of Japan
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Abstract

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We investigate the sputtering and thermal desorption of various grain-surface species in one dimensional steady-state shock models motivated by the recent detection of SO emission towards class 0-I protostars. We find that the thermal desorption is more efficient at higher densities, while the efficiency of sputtering is independent of density. SO is completely desorbed, if the accretion velocity is higher than ~ 2 km s−1 and ~ 4 km s−1, with the pre-shock density of 109 cm−3 and 108 cm−3, respectively. The column density of warm post-shock gas is found to be N ~ 1021 cm−2. If the abundance of SO ice is ~ 10−7 relative to hydrogen in the pre-shock material, SO emission around L1527 can be explained by the sublimation at the accretion shock.

Keywords

astrochemistryprotoplanetary disk
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , E1
Copyright
Copyright © International Astronomical Union 2015 

References

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