Supernova precursors

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Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978mmsai..49..389r&link_type=abstract

(Società Astronomica Italiana and Consiglio Nazionale delle Ricerche, Workshop on Supernovae and Supernova Remnants, 1st, Erice,

Astronomy and Astrophysics

Astrophysics

10

Giant Stars, O Stars, Stellar Winds, Supergiant Stars, Supernovae, Astrophysics, B Stars, Carbon Stars, Supernova Remnants

Scientific paper

Observational evidence for stellar winds from OB stars and late-type giants and supergiants is reviewed. Some properties of massive stars and of intermediate-mass stars are discussed which are of relevance to the supernova (SN) phenomenon. A relation between degenerate carbon ignition and type I SN is considered, and SN environments are examined. It is suggested that at the moment of a SN outburst the exploding star is embedded not in a 'normal' homogeneous interstellar medium (ISM), but rather in an environment produced by a stellar wind in the past history of the star and by the stellar-wind interaction with the ISM. Three phases in the evolution of a supernova remnant (SNR) are distinguished: (1) the early, or light-curve, phase, which persists for a few years after the SN explosion; (2) the young SNR phase, which lasts a few thousand years and during which the original ejecta are still observable; and (3) the old SNR phase.

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