Physics
Scientific paper
Apr 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988natur.332..514c&link_type=abstract
Nature (ISSN 0028-0836), vol. 332, April 7, 1988, p. 514-516. NSF-NASA-supported research.
Physics
39
Gas-Ion Interactions, Plasma Interactions, Stellar Envelopes, Stellar Winds, Supernova 1987A, Blue Stars, Red Giant Stars, Ultraviolet Spectra
Scientific paper
Although the progenitor of supernova 1987A apparently was a blue supergiant, there is theoretical and observational evidence for an earlier red supergiant phase. The fast wind from the blue star is expected to drive a shell into the slow, dense red supergiant wind. Observed narrow ultraviolet lines are probably from shell gas that was photoionized by the initial radiation burst from the supernova. The light travel time effects on the evolution of the line fluxes, line profiles and spatial structure of the emission are described. Current high spectral resolution observations suggest a lower limit to the age of the shell of 5,000 yr and suggest a relatively low shell velocity. The narrow lines are predicted to shift to the red at a rate depending on the shell age. Observations of X rays below 10 keV are difficult to interpret in terms of circumstellar interaction.
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