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Radio Emission from SN 1988Z and Very Massive Star Evolution

C. L. Williams·N. Panagia·S. D. Van Dyk·C. K. Lacey·K. W. Weiler·R. A. Sramek
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Abstract

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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C. L. Williams, N. Panagia, S. D. Van Dyk, C. K. Lacey, K. W. Weiler, R. A. Sramek. 2002-08-08. Radio Emission from SN 1988Z and Very Massive Star Evolution. https://doi.org/10.1086/344087

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