Final mixing in extreme horizontal branch stars

Details Final mixing in extreme horizontal branch stars Final mixing in extreme horizontal branch stars

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232...67c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 1, June 1990, p. 67-69.

Astronomy and Astrophysics

Astronomy

10

Blue Stars, Horizontal Branch Stars, Mixing, Stellar Envelopes, Stellar Evolution, Ultraviolet Radiation, Abundance, Chemical Reactions, Ultraviolet Astronomy

Scientific paper

When the hydrogen-rich envelope of an evolved horizontal branch structure is too small, with envelope mass not greater than 0.02 M(0), to allow the development of the asymptotic giant branch phase, a final helium-shell flash develops when the star is already on its white dwarf cooling sequence. The flash is strong enough to reach the hydrogen-rich layers. Substantial mixing and/or envelope ejection follow, together with some neutron nucleosynthesis.

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