Computer Science – Numerical Analysis
Scientific paper
Jun 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232...31x&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 1, June 1990, p. 31-36.
Computer Science
Numerical Analysis
16
A Stars, B Stars, Convection, F Stars, Stellar Envelopes, Stellar Models, Boundary Conditions, Ionized Gases, Numerical Analysis, Peculiar Stars, Stellar Temperature
Scientific paper
Four models of the convective envelope of B-F stars are calculated using the nonlocal theory of convection. They fall clearly into two groups, a hotter one and a cooler one. The hotter stars with effective temperatures over 7000 K have two separate convectively unstable regions in the ionized hydrogen and in the second ionized helium regions, which are linked by overshooting when the convective parameters are greater than 0.75. The bottom temperature T(b) of the convective zone is about 56,000 K and its total mass is about 5 x 10 to the 24th g, which are almost independent of T(e). When the effective temperature T(e) of stars becomes smaller than about 7000 K, the convective zone deepens inward abruptly and its total mass increases sharply with decreasing T(e). Convective instability in the P(g)-T plane is studied in detail. It is shown that the Peclet number P(e) is also important not only for the efficiency of convective energy transport but also for the extension of the convective zone.
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