Astron. Astrophys. Suppl. Ser. 138, 467-468
M.H. Wieringa1 - S.R. Kulkarni2 - D.A. Frail3
Send offprint request: D.A. Frail
1 - Australia Telescope National Facility, CSIRO, Epping 2121, Australia
2 - Division of Physics, Mathematics, and Astronomy 105-24, California Institute of Technology, Pasadena, CA 91125, U.S.A.
3 - National Radio Astronomy Observatory (NRAO), Socorro, NM 87801, U.S.A.
Received January 21; accepted June 9, 1999
SN1998bw shot to fame by claims of association with GRB980425.
Independent of its presumed association with a GRB, this SN is unusual
in its radio
properties. A simple interpretation of the unusually
bright radio emission leads us to the conclusion that there are two
shocks in this SN: a slow moving shock containing most of the ejecta
and a relativistic shock () which is responsible for the
radio emission. This is the first evidence for the existence of
relativistic shocks in supernovae. It is quite plausible that this
shock may produce high energy emission (at early times and by inverse
Compton scattering). As with other supernovae, we expect radio
emission at much later times powered primarily by the slow moving
ejecta. This expectation has motivated us to continue monitoring this
Key words: gamma-ray: bursts
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