A lower limit to the mass of the supernova that produced N 63 A

Details A lower limit to the mass of the supernova that produced N 63 A A lower limit to the mass of the supernova that produced N 63 A

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980pasp...92...32v&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 92, Feb.-Mar. 1980, p. 32-35.

Astronomy and Astrophysics

Astronomy

9

O Stars, Star Clusters, Stellar Luminosity, Stellar Mass, Supernova Remnants, Astronomical Photography, Cosmology, Electrophotometry, Stellar Models

Scientific paper

The LMC supernova remnant N 63 A is located near the center of the small association NGC 2030. Observations of the most luminous association member, combined with evolutionary models incorporating conservative mass-loss rates, yield a mass of 30 solar masses for the brightest star in NGC 2030. Since association members are approximately coeval the supernova precursor must have had a mass not less than 30 solar masses. Both the optical morphology and the radio spectral index of N 63 A show that it is not a plerionic SNR. This provides a counter example to the suggestion that massive O-type stars are the progenitors of Crab-like remnants.

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