Dynamic phases in the evolution of a 1.25 solar mass C-O star

Details Dynamic phases in the evolution of a 1.25 solar mass C-O star Dynamic phases in the evolution of a 1.25 solar mass C-O star

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..37..463k&link_type=abstract

Astrophysics and Space Science, vol. 37, Oct. 1975, p. 463-476.

Astronomy and Astrophysics

Astrophysics

4

Dynamic Stability, Nuclear Fusion, Stellar Evolution, White Dwarf Stars, Abundance, Astronomical Models, Carbon, Convective Flow, Oxygen, Stellar Mass

Scientific paper

The evolution of a 1.25 solar mass carbon and oxygen (equal fractions by mass) homogeneous star is followed by means of a computer code capable of dealing with dynamic evolutionary phases. After carbon ignition at the center, followed by successive shell flashes and the formation of a T-inversion, convection begins at the surface and the model evolves through a very short but strong dynamic phase (a pulsation) after which it settles down to a white dwarf configuration.

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