Thermal instabilities in low-mass subgiants?

Details Thermal instabilities in low-mass subgiants? Thermal instabilities in low-mass subgiants?

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..840v&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 15, 1988, p. 840-850. NSERC-supported research.

Astronomy and Astrophysics

Astrophysics

25

Stellar Luminosity, Stellar Mass, Stellar Models, Subgiant Stars, Thermal Instability, Globular Clusters, Red Giant Stars, Stellar Evolution, Stellar Interiors, Stellar Rotation, Stellar Structure

Scientific paper

The thermal stability of evolving stars in globular clusters has been examined in order to determine whether or not gaps and the observationally inferred deep mixing near the base of the red-giant branch can be explained in terms of an instability of the hydrogen-burning shell. The results of this investigation are that, in agreement with previous suggestions, the greatest potential for such an instability occurs just at the point where a star begins to ascend the giant branch - i.e., where gaps are seen in some systems - but, in contrast with earlier predictions, the standard models do not actually become unstable. However, from all indications, the stability is believed to be marginal, and it is suggested that rotation, which has now been observed in some globulars, may be the mechanism by which an instability is produced.

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