Carbon ignition and burning in degenerate stellar cores

Details Carbon ignition and burning in degenerate stellar cores Carbon ignition and burning in degenerate stellar cores

Mar 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...196..791c&link_type=abstract

Astrophysical Journal, vol. 196, Mar. 15, 1975, pt. 1, p. 791-803.

Astronomy and Astrophysics

Astrophysics

53

Carbon 12, Neutrinos, Nuclear Fusion, Stellar Cores, Stellar Evolution, Energy Conversion, Stellar Envelopes, Stellar Mass, Stellar Temperature

Scientific paper

The investigation is concerned with the evolution of a hypothesized set of stars with masses from four to eight times the solar mass. The stars considered neither lose their envelope nor ignite carbon in a nondegenerate central zone. Following core helium burning, a temperature inversion occurs in the central region. Because of the decrease in temperature, the core evolves to very high densities before carbon ignition takes place. The investigation shows that the convective Urca process suggested by Paczynski (1972) as a means to control the carbon burning is a tremendously efficient radiator of energy.

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