Mimicking semi-convection by convective overshooting

Details Mimicking semi-convection by convective overshooting Mimicking semi-convection by convective overshooting

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...240..305c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 240, no. 2, Dec. 1990, p. 305-307.

Statistics

Computation

8

Computational Astrophysics, Convection, Horizontal Branch Stars, Stellar Cores, Stellar Evolution, Stellar Structure, Abundance, Algorithms, Computer Programs, Helium, Stellar Composition

Scientific paper

This paper investigates the behavior of so called 'semiconvection' (described by Schwarzschild, 1970; Castellani et al., 1971), of stars burning He in a convective core but exibiting an apparent spontaneous capability to partially mix into the core the matter from outside the formal boundaries of the convective region. A simple numerical algorithm based on a small and ad hoc amount of convective overshooting is presented which, if properly tuned, can mimick the effect of semiconvection in the computation of those stellar evolutionary phases in which a convective helium burning core is present. Using this algorithm, the time-consuming numerical procedures involved in the evaluation of the correct chemical profiles at the boundaries of the formally convective He core can be avoided.

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