Advanced evolutionary phases of large-metallicity low-mass stars and the problem of the ultraviolet excess of elliptical galaxies

Details Advanced evolutionary phases of large-metallicity low-mass stars and the problem of the ultraviolet excess of elliptical galaxies Advanced evolutionary phases of large-metallicity low-mass stars and the problem of the ultraviolet excess of elliptical galaxies

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...381..393c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 381, Nov. 10, 1991, p. 393-408.

Astronomy and Astrophysics

Astronomy

51

Elliptical Galaxies, Metallicity, Stellar Mass, Ultraviolet Astronomy, Abundance, Asymptotic Giant Branch Stars, Star Distribution, Stellar Evolution, Stellar Interiors

Scientific paper

A set of evolutionary tracks of large-metallicity low-mass stars, covering the advanced evolutionary phases from the zero-age horizontal branch to the final white dwarf cooling phase, at the onset of crystallization, are presented. Physical parameters of the evolved stars were selected to search for models leaving the AGB phase before the onset of the thermal pulses and evolving to the blue side of the H-R diagram according to an evolutionary scheme earlier defined as post-early AGB evolution. The maximum UV flux that post-AGB models can provide is found to be insufficient to account for the UV emission of most UV-emitting elliptical galaxies, whereas models following the post-EAGB evolutionary behavior produce much more UV flux. Among the star models evolving off the early AGB, before the onset of thermal pulses, those maximizing the production of the UV flux give enough UV light to explain even the most UV-upturned branches observed in the spectra of the most metal-rich elliptical galaxy.

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