SN 1993J: The early radio emission and evidence for a changing presupernova mass-loss rate

Details SN 1993J: The early radio emission and evidence for a changing presupernova mass-loss rate SN 1993J: The early radio emission and evidence for a changing presupernova mass-loss rate

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432l.115v&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 432, no. 2, p. L115-L118

Mathematics

Metric Geometry

103

Flux Density, Radio Emission, Shock Wave Interaction, Solar Wind Velocity, Stellar Winds, Supernovae, Light Curve, Radio Spectra, Stellar Envelopes, Very Large Array (Vla)

Scientific paper

We present daily-to-weekly monitoring of the first 8 months of radio emission from supernova (SN) 1993J using the Very Large Array (VLA) at five wavelengths, providing the most detailed radio light curves ever established for an SN. While the radio emission evolves regularly in both time and frequency, the usual form of the SN shock/circumstellar medium interaction model does not adequately describe the observations. In particlar, for a spherically symmetric geometry, the circumstellar density profile is flatter (rhoCSM proportional to r-1.5) than that (rhoCSM proportional to r-2) generally assumed for a constant mass-loss rate, constant-velocity stellar wind. This is interpreted as a decrease in the pre-SN mass-loss rate (or increase in wind velocity) immediately prior to explosion. Additionally, the rate of increase in the early radio emission at each frequency cannot simply be described as due to decreasing external absorption by a uniform medium, but requires the presence of higher density 'clumps' or 'filaments' embedded in the stellar wind.

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