Model for R Coronae Borealis stars

Details Model for R Coronae Borealis stars Model for R Coronae Borealis stars

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aj....102..284w&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 102, July 1991, p. 284-288.

Astronomy and Astrophysics

Astronomy

13

R Coronae Borealis Stars, Stellar Evolution, Stellar Interiors, Stellar Models, Abundance, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

An evolutionary model is proposed in which R Coronae Borealis stars are in a second common-envelope phase, with a low-mass companion orbiting well inside the envelope. The high mass-loss rate in the first common-envelope phase turns the massive star into a hydrogen-deficient star. In the second common-envelope phase, as a result of shear induced by the inner envelope rotation and possibly by excited gravity-wave-induced turbulence, carbon and oxygen are being dredged up from the core into the envelope. This evolutionary scenario smoothly connects R CrB stars to the double-mass-loss-episodes evolutionary scenario of hydrogen-deficient binaries suggested by Plavec (1973). This model may have consequences for the nature of mass loss in R Coronae Borealis stars: the orbiting companion breaks spherical symmetry allowing for nonradial pulsations and asymmetric mass loss. The optical polarization and IR observations may point to axisymmetric mass loss with the same axis of symmetry for the different mass-loss episodes.

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