Helium-rich supernovas

Details Helium-rich supernovas Helium-rich supernovas

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987sciam.257...50w&link_type=abstract

Scientific American (ISSN 0036-8733), vol. 257, Nov. 1987, p. 50-58.

Computer Science

2

Computerized Simulation, Helium, Stellar Evolution, Supernovae, Explosions, Gravitational Collapse, Light Curve, Line Spectra, Oxygen, Spectrum Analysis, Stellar Models

Scientific paper

The spectra of type Ib supernovas are described and explained in terms of the explosions of stars of less than 25 solar masses which have massive binary companions. The spectral evidence, radio observations, and observed association with H II regions all suggest that supernovas of this new class originate as massive stars. The helium feature in their spectra indicates that the progenitor stars are not massive enough to blow off their envelopes; thus, a massive companion is required to pull the envelope off, after which the core explodes.

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