Radio studies of extragalactic supernovae

Details Radio studies of extragalactic supernovae Radio studies of extragalactic supernovae

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sci...231.1251w&link_type=abstract

Science (ISSN 0036-8075), vol. 231, March 14, 1986, p. 1251-1254.

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2

Astronomical Models, Extragalactic Radio Sources, Radio Emission, Supernovae, Nonthermal Radiation, Radio Spectra, Shock Waves, Stellar Winds, Synchrotron Radiation

Scientific paper

The theoretical understanding of centimeter radio emission spectra from supernovae is examined and observational data since 1980 are discussed. After the explosion, supernovae quickly become detectable in the radio range, first at shorter wavelengths, and later at progressively longer wavelengths. Data support the model of a gradually decreasing amount of thermal ionized absorbing gas surrounding the radio-emitting regions as the shock travels outward, and a corresponding decrease in the optical depth. It is suggested that the absorbing material is mass lost from the presupernova system in the last stages of evolution before the explosion. The radio emission is of nonthermal synchrotron origin, and is generated either externally by the shock wave propagating through a high density stellar wind (the 'minishell' model), or internally by pulsar acceleration from the supernova stellar remnant (the 'miniplerion' model). The mathematical formulation to curve-fit flux density/time data for the Type I (SL) supernova SN1983n corresponds quite well to the minishell model. Other patterns include the Type II supernovae showing consistently flatter nonthermal radio spectral index, and a slower decline of flux density with time, than the Type I supernovae.

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