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An Update on Radio Supernovae

Published online by Cambridge University Press:  12 April 2016

Schuyler D. Van Dyk ,
Richard A. Sramek ,
Kurt W. Weiler ,
Marcos J. Montes  and
Nino Panagia
Schuyler D. Van Dyk
Affiliation:
Dept. Phys & Astr., UCLA, Los Angeles, CA 90095
Richard A. Sramek
Affiliation:
National Radio Astronomy Observatory, Socorro, NM 87801, U.S.A.
Kurt W. Weiler
Affiliation:
Code 7214, Naval Research Lab, Washington, DC 20375-5320, U.S.A.
Marcos J. Montes
Affiliation:
Code 7214, Naval Research Lab, Washington, DC 20375-5320, U.S.A.
Nino Panagia
Affiliation:
STScI, Baltimore, MD 21218, U.S.A.

Abstract

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The radio emission from supernovae (SNe) is nonthermal synchrotron radiation of high brightness temperature, with a “turn-on” delay at longer wavelengths, power-law decline after maximum with index β, and spectral index α asymptotically decreasing with time to a final, optically thin value. Radio supernovae (RSNe) are best described by the Chevalier (1982) “mini-shell” model, with modifications by Weiler et al. (1990). RSNe observations provide a valuable probe of the SN circumstellar environment and constraints on progenitor masses. We present a progress report on a number of recent RSNe, as well as on new behavior from RSNe 1979C and 1980K, and on RSNe as potential distance indicators. In particular, we present updated radio light curves for SN 1993J in M81.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 357 - 358
Copyright
Copyright © Astronomical Society of the Pacific 1998

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