Radio Emission from SN 1988Z and Very Massive Star Evolution

Details Radio Emission from SN 1988Z and Very Massive Star Evolution Radio Emission from SN 1988Z and Very Massive Star Evolution

2002-08-08

arxiv.org/abs/astro-ph/0208190v1

Astrophys.J. 581 (2002) 396-403

Astronomy and Astrophysics

Astrophysics

11 pages, 3 figures, ApJ, in press (2002 Dec 10)

Scientific paper

10.1086/344087

We present observations of the radio emission from the unusual SN 1988Z made with the VLA from 385 to 4,438 days after explosion. SN 1988Z is the most distant radio supernova ever detected. The radio light curves are well-described by a model involving the blastwave interacting with a high-density circumstellar cocoon, which consists almost entirely of clumps or filaments. However, at age ~ 1750 days the SN declines much more rapidly than expected, without a change in absorption parameters. This is due to a change in the number density of circum- stellar clumps without a change in the average properties of each clump. This also represents a change in the presupernova stellar wind properties ~ 10,000 yr before explosion. A massive wind (Mdot >~ 10^{-4} Msun/yr) and very high ZAMS mass, ~ 20--30 Msun, is implied for the SN progenitor, similar to what is likely the case for SNe 1986J and 1998bw.

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