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An interpretation of the overionized plasma in supernova remnant W49B

Published online by Cambridge University Press:  29 January 2014

Xin Zhou ,
Marco Miceli ,
Fabrizio Bocchino ,
Salvatore Orlando ,
Yang Chen ,
Li Ji  and
Ji Yang
Xin Zhou
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences Nanjing 210008, China Key Laboratory of Radio Astronomy, Chinese Academy of Sciences Nanjing 210008, China Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education Nanjing 210093, China
Marco Miceli
Affiliation:
Dipartimento di Fisica, Universit di Palermo Piazza del Parlamento 1, I-90134 Palermo, Italy INAF-Osservatorio Astronomico di Palermo Piazza del Parlamento 1, I-90134 Palermo, Italy
Fabrizio Bocchino
Affiliation:
INAF-Osservatorio Astronomico di Palermo Piazza del Parlamento 1, I-90134 Palermo, Italy
Salvatore Orlando
Affiliation:
INAF-Osservatorio Astronomico di Palermo Piazza del Parlamento 1, I-90134 Palermo, Italy
Yang Chen
Affiliation:
Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education Nanjing 210093, China Department of Astronomy, Nanjing University Nanjing 210093, China
Li Ji
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences Nanjing 210008, China
Ji Yang
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences Nanjing 210008, China
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Abstract

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W49B is a mixed-morphology supernova remnant (SNR) with the presence of enhanced abundances and overionization confirmed by X-ray observation. For the overionization, a strong radiative recombination continuum (RRC) has been detected and confirmed by SUZAKU and XMM-Newton. Here, we investigate these intriguing observational results through a multidimensional hydrodynamic model that takes into account, for the first time, the mixing of ejecta with the circumstellar and interstellar medium, thermal conduction, and non-equilibrium ionization. The model can reproduce the morphology and the overionization pattern of W49B. We found that the overionized plasma originates from the rapid cooling of the hot plasma originally heated by the shock reflected from the dense ring-like cloud. In addition, based on the most updated ATOMDB (v2.0.2), we calculated the spectrum of one cell in the overionized region from the simulation results at present. We got the overionized spectrum that is in agreement with the observational results. Thus, our primary result indicates that the model is consistent with the observations both spatially and spectrally.

Keywords

hydrodynamicsmethods: numericalISM: individual: W49B(G43.3-0.2)supernova remnantX-rays: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S296: Supernova Environmental Impacts , January 2013 , pp. 364 - 365
Copyright
Copyright © International Astronomical Union 2014 

References

Keohane, J. W., Reach, W. T., Rho, J., & Jarrett, T. H. 2007, ApJ, 654, 938CrossRefGoogle Scholar
Miceli, M., Bocchino, F., Decourchelle, A., Ballet, J., & Reale, F. 2010, A&A, 514, L2Google Scholar
Miceli, M., Decourchelle, A., Ballet, J., Bocchino, F., Hughes, J. P., Hwang, U., & Petre, R. 2006, A&A, 453, 567Google Scholar
Rho, J. & Petre, R. 1998, ApJ, 503, L167CrossRefGoogle Scholar
Ozawa, M., Koyama, K., Yamaguchi, H., Masai, K., & Tamagawa, T. 2009, ApJ, 706, L71Google Scholar
Zhou, X., Miceli, M., Bocchino, F., Orlando, S., & Chen, Y. 2011, MNRAS, 415, 244CrossRefGoogle Scholar