Low-mass stars. I - Flash-driven luminosity and radius variations. II - The core mass-luminosity relations. III - Low-mass stars with steady mass loss - Up to the asymptotic giant branch and through the final thermal pulses

Details Low-mass stars. I - Flash-driven luminosity and radius variations. II - The core mass-luminosity relations. III - Low-mass stars with steady mass loss - Up to the asymptotic giant branch and through the final thermal pulses Low-mass stars. I - Flash-driven luminosity and radius variations. II - The core mass-luminosity relations. III - Low-mass stars with steady mass loss - Up to the asymptotic giant branch and through the final thermal pulses

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..632b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 632-670.

Other

80

Late Stars, Stellar Cores, Stellar Interiors, Stellar Luminosity, Stellar Mass, Variable Stars, Light Curve, Metallic Stars, Planetary Nebulae, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

The observable and potentially observable consequences of helium shell flashes were investigated for a number of low-mass stars. Stars of low metallicity (Z = 0.001) with initial masses of 1.0 Msun, 1.2 Msun, and 2.0 Msun were considered, as well as stars of solar metallicity (Z = 0.02) with initial masses of 1.2 Msun and 3.0 Msun. For flashes whose strength was at or near maximum amplitude, light curves and radius curves were obtained over the full flash cycle. These are of interest to investigations of envelope instability and mass ejection. Potentially observable luminosity variations are confined to a few decades immediately following the helium shell flash,as compared to interflash periods of tens of thousands of years, and so would be exhibited by less than one AGB star in a thousand; radius variations would be even harder to observe directly. The slower variations, however, cause stars of initial mass near 1.0 Msun to spend as much as 20%-30% of the interflash period at a luminosity a factor of 2 lower than the interflash luminosity indicated by the Mc-L relation. Higher mass stars stay closer to the Mc-L line. Particularly for the low-metallicity cases, the postflash luminosity maximum causes the star to spend a few centuries at a luminosity as much as twice that indicated by the Mc-L relation. This could cause the star to encounter dynamic envelope instability and rapid mass loss at a core mass lower by of order ΔMc≍ 0.1 Msun than would otherwise be the case.

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