Physics
Scientific paper
Nov 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989natur.342..403a&link_type=abstract
Nature (ISSN 0028-0836), vol. 342, Nov. 23, 1989, p. 403-405.
Physics
22
Abundance, Stellar Evolution, Stellar Winds, Supernova 1987A, Emission Spectra, Helium, Infrared Spectroscopy, Stellar Envelopes
Scientific paper
To explain why the progenitor of supernova 1987A exploded as a blue supergiant star, models of stellar evolution require that there must have been extensive mixing into the hydrogen-rich envelope of materials from deeper, helium-rich regions. Estimates of the helium abundance in the outer layers, which can be obtained from infrared spectroscopy of the stellar wind from the progenitor, can help to determine the extent of the mixing. The initial ultraviolet flash from the surface of the supernova indicated electron densities of about 10,000/cu cm, far greater than expected for the wind shed by the precursor star in either its blue supergiant or preceding red supergiant phase. However, the interaction of the two winds could produce a shell of the requisite density. From observations of the infrared helium triplet at 1083 nm, it is inferred that the red supergiant wind was strongly asymmetric and that part of its had a high helium abundance.
Allen David A.
Meikle Peter S. W.
Spyromilio Jason
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