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Low Frequency Radio and X-ray Properties of Core-Collapse Supernovae

Published online by Cambridge University Press:  19 September 2016

A. Ray ,
P. Chandra ,
F. Sutaria  and
S. Bhatnagar
A. Ray
Affiliation:
Tata Institute of Fundamental Research, Mumbai, India;[email protected]
P. Chandra
Affiliation:
Tata Institute of Fundamental Research, Mumbai, India;[email protected] Joint Astronomy Program, Indian Inst. Science, Bangalore, India;[email protected]
F. Sutaria
Affiliation:
Physics Dept., Technical University Munich, Germany;[email protected]
S. Bhatnagar
Affiliation:
National Centre for Radio Astrophysics, TIFR, Pune, India National Radio Astronomy Observatory, Socorro, USA;[email protected]

Summary

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Radio and X-ray studies of young supernovae probe the interaction between the supernova shock waves and the surrounding medium and give clues to the nature and past of the progenitor star. Here we discuss the early emission from type Ic SN 2002ap and argue that repeated Compton boosting of optical photons by hot electrons presents the most natural explanation of the prompt X-ray emission. We describe the radio spectrum of another type Ic SN 2003dh (GRB030329) obtained with combined GMRT and VLA data. We report on the low frequency radio monitoring of SN 1995N and our objectives of distinguishing between competing models of X-ray emission from this SN and the nature of its progenitor by X-ray spectroscopy. Radio studies on SN 2001gd, SN 2001ig and SN 2002hh are mentioned.

Type
Part II Supernovae: Observations
Information
International Astronomical Union Colloquium , Volume 192: Cosmic Explosions , 2005 , pp. 145 - 150
Copyright
Copyright © Springer-Verlag 2005

References

1. Berger, E., Kulkami, S., Chevalier, R.A.: Astrophys. J. Lett. 577,L5 (2002)Google Scholar
2. Berger, E. et al.: astro-ph 0308187 (2003)Google Scholar
3. Chevalier, R.A., С. Fransson: Astrophys. J. 420, 268 (1994)Google Scholar
4. Chugai, N.N.: Astrophys. J. Lett. 414, L101 (1993)Google Scholar
5. Fox, D.W. et al.: Mori. Not. R. Astron. Soc. 319, 1154 (2000)Google Scholar
6. Fransson, C.: Astron. Astrophys. 111, 140 (1982)Google Scholar
7. Hjorth, J. et al.: Nature 423, 847 (2003)Google Scholar
8. Immler, S., Lewin, W.H.G.: In: Supernovae and Gamma-Ray Bursters, ed. Weiler, K. (Springer: Berlin, 2002) pp. 91–112 Google Scholar
9. Mazzali, P. et al.: Astrophys. J. Lett. 572, L61 (2002)Google Scholar
10. Nakano, S., Kushida, R., Li, W.: IAUC 7810 (2002)Google Scholar
11. Pooley, D. et al.: Astrophys. J. 572, 932 (2002)Google Scholar
12. Pozdnyakov, L., Soboi, I., Sunyaev, R.: Sov. Astron. 21, 708 (1977)Google Scholar
13. Sutaria, F., Chandra, P., Bhatnagar, S., Ray, A.: Astron. Astrophys. 397, 1011 (2003)CrossRefGoogle Scholar
14. Zimmermann, H.-U., Aschenbach, B.: Astron. Astrophys. 406, 969 (2003)CrossRefGoogle Scholar