Novae, supernovae, and neutron sources

Details Novae, supernovae, and neutron sources Novae, supernovae, and neutron sources

Jun 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...198l.113s&link_type=abstract

Astrophysical Journal, vol. 198, June 15, 1975, pt. 2, p. L113-L117.

Astronomy and Astrophysics

Astrophysics

8

Neutron Emission, Novae, Nuclear Fusion, Stellar Evolution, Supernovae, White Dwarf Stars, Astronomical Models, Neutron Flux Density, Nuclear Capture, Shock Wave Propagation, Stellar Mass Ejection

Scientific paper

The evolution of thermonuclear runaways is examined in two models of white dwarfs with extreme enhancements of C-12 in their envelopes to test the predictions of Hoyle and Clayton (1974) that novae will result from such stars and a large neutron flux will be produced. In agreement with these predictions, it is assumed that the large amount of C-12 is due to the accretion of hydrogen-rich material from a disk surrounding a carbon-oxygen white dwarf. The evolution of the two models is described in detail, and the results suggest that accretion of hydrogen-rich material will always result in a thermonuclear runaway, although mass ejection will not occur unless CNO nuclei are enhanced. It is noted that one model produces a substantial neutron flux for a short time which is sufficient to drive an intermediate neutron-capture process.

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