On convective and semiconvective mixing in massive stars

Details On convective and semiconvective mixing in massive stars On convective and semiconvective mixing in massive stars

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237..900c&link_type=abstract

Astrophysical Journal, Part 1, vol. 237, May 1, 1980, p. 900-902.

Astronomy and Astrophysics

Astrophysics

46

Main Sequence Stars, Stellar Evolution, Stellar Mass, Supermassive Stars, Convection, Statistical Analysis, Stellar Interiors, Stellar Luminosity, Stellar Models, Turbulence Effects

Scientific paper

The evolutionary sequence of a 15.57-solar mass star made with a simplified turbulence transport model demonstrates the importance of accurately modeling the turbulent convection in the stellar interior. The combination of the self-diffusion of turbulence and its finite decay time in a stable region extend the convective core by about 3 solar masses, profoundly affecting the evolution of the star. Among the important effects are the elimination of semiconvection and the increase in both the lifetime and luminosity in the hydrogen-burning phase.

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