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MHD Simulation of Supernova Remnants

Published online by Cambridge University Press:  17 October 2017

D. Wu ,
M. F. Zhang ,
S. S. Shan  and
W. W. Tian
D. Wu
Affiliation:
Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected] College of Information Science and Technology, Beijing Normal University, Beijing 100875, China
M. F. Zhang
Affiliation:
Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected] School of Astronomy and Space Science, University of Chinese Academy of Sciences, 19A Yuquan Road, Shijingshan District, Beijing 100049, China
S. S. Shan
Affiliation:
Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected] School of Astronomy and Space Science, University of Chinese Academy of Sciences, 19A Yuquan Road, Shijingshan District, Beijing 100049, China
W. W. Tian
Affiliation:
Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected] Department of Physics & Astronomy, University of Calgary, Calgary, Alberta T2N 1N4, Canada
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Abstract

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We present some Magnetohydrodynamic (MHD) simulations for supernova remnants (SNRs), which hints the thicknesses of SNRs’ shells are likely related to the density and density distribution of surrounding interstellar medium (ISM). The simulations show clear formation and evolution of reverse shocks. In addition, we find that stellar winds can blow a bubble around the progenitor stars then lead to weaker radio emission at the center of SNRs.

Keywords

Methods: numericalISM: supernova remnantsMHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 174 - 177
Copyright
Copyright © International Astronomical Union 2017 

References

Denis, A. Leahy & Jacqueline, Williams 2017, AJ, 153, 239 Google Scholar
Jackson, J. M., Rathborne, J. M., Shah, R. Y., Simon, R., Bania, T. M., Clemens, D. P., Chambers, E. T., Johnson, A. M., Dormody, M., Lavoie, R., & Heyer, M. H. 2006 ApJS, 163, 145 Google Scholar
Jun, B.-I. & Norman, M. L. 1996, ApJ, 465, 800 CrossRefGoogle Scholar
Koo, B.-C. & Moon, D.-S. 1997, ApJ, 475, 194 Google Scholar
Lamers, H. J. G. L. M. & Cassinelli, J. P. 1999, Introduction to Stellar Winds CrossRefGoogle Scholar
Mignone, A., Bodo, G., Massaglia, S., Matsakos, T., Tesileanu, O., Zanni, C., & Ferrari, A. 2007, ApJS, 170, 228 Google Scholar
Orlando, S., Bocchino, F., Reale, F., Peres, G., & Petruk, O. 2007, A&A, 470, 927 Google Scholar