Nitrogen and helium enhancement in the progenitor of supernova 1987A

Details Nitrogen and helium enhancement in the progenitor of supernova 1987A Nitrogen and helium enhancement in the progenitor of supernova 1987A

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988natur.334..508s&link_type=abstract

Nature (ISSN 0028-0836), vol. 334, Aug. 11, 1988, p. 508-510.

Computer Science

55

Emission Spectra, Helium, Nitrogen, Stellar Envelopes, Stellar Evolution, Supernova 1987A, Blue Stars, Stellar Mass, Supergiant Stars

Scientific paper

Recent ultraviolet observations of SN 1987A indicate that the ultraviolet emissions come from circumstellar material which was processed by hydrogen burning in the interior and ejected into space when the progenitor was a red supergiant. The progenitor of SN 1987A must therefore have evolved first to a red supergiant and then back to the blue. From calculations of massive star evolution, it is shown here how the star could have undergone blue-red-blue evolution. By comparing these theoretical models with the abundance information from the ultraviolet observations, it is concluded that the hydrogen-rich envelope of the progenitor was as massive as 7-11 solar masses and that almost the whole envelope was uniformly mixed, probably because of rapid rotation.

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