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Molecular Environments of Supernova Remnants†

Published online by Cambridge University Press:  29 January 2014

Yang Chen ,
Bing Jiang ,
Ping Zhou ,
Yang Su ,
Xin Zhou ,
Hui Li  and
Xiao Zhang
Yang Chen
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected], [email protected], [email protected], [email protected] Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China
Bing Jiang
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected], [email protected], [email protected], [email protected]
Ping Zhou
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected], [email protected], [email protected], [email protected]
Yang Su
Affiliation:
Purple Mountain Observatory, 2 West Beijing Road, Nanjing 210008, China email: [email protected], [email protected]
Xin Zhou
Affiliation:
Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China Purple Mountain Observatory, 2 West Beijing Road, Nanjing 210008, China email: [email protected], [email protected]
Hui Li
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected], [email protected], [email protected], [email protected] Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA email: [email protected]
Xiao Zhang
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected], [email protected], [email protected], [email protected]
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Abstract

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There are about 70 Galactic supernova remnants (SNRs) that are now confirmed or suggested to be in physical contact with molecular clouds (MCs) with six kinds of evidence of multiwavelength observations. Recent detailed CO-line spectroscopic mappings of a series of SNRs reveal them to be in cavities of molecular gas, implying the roles the progenitors may have played. We predict a linear correlation between the wind bubble sizes of main-sequence OB stars in a molecular environment and the stellar masses and discuss its implication for supernova progenitors. The molecular environments of SNRs can serve as a good probe for the γ-rays arising from the hadronic interaction of the accelerated protons, and this paper also discusses the γ-ray emission from MCs illuminated by diffusive protons that escape from SNR shocks.

Keywords

ISM: supernova remnantsISM: cloudsISM: bubblesISM: moleculesgamma-rays: ISMstars: early-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S296: Supernova Environmental Impacts , January 2013 , pp. 170 - 177
Copyright
Copyright © International Astronomical Union 2014 

Footnotes

†

Supported by the 973 Program grant 2009CB824800, the NSFC grants 11233001, 11103082, and 11203013, grants 20120091110048 and 20110091120001 from the Educational Ministry of China, and grant 2011M500963 from the China Postdoctoral Science Foundation.

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