Convective mixing in helium white dwarfs

Details Convective mixing in helium white dwarfs Convective mixing in helium white dwarfs

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230..563v&link_type=abstract

Astrophysical Journal, Part 1, vol. 230, June 1, 1979, p. 563-569. Research supported by the Natural Sciences and Engineering R

Astronomy and Astrophysics

Astrophysics

22

Convective Flow, Helium, Stellar Atmospheres, Turbulent Mixing, White Dwarf Stars, Carbon, Stellar Envelopes, Stellar Models

Scientific paper

The conditions under which convective mixing episodes take place between the helium envelopes and the underlying carbon layers in helium-rich white dwarfs are investigated. It is found that, for essentially any value of the initial helium content less than the maximum mass a helium convection zone can have, mixing does occur and leads, in the vast majority of cases, to an almost pure carbon superficial composition. Mixing products that show only traces of carbon while retaining helium-dominated envelopes are possible only if the initial helium content is quite close to the maximum possible mass of the helium convection zone. In the presence of turbulence, this restriction could be relaxed, however, and the helium-rich 4670-A stars may possibly be explained in this fashion.

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