Clues on the hot star content and the ultraviolet output of elliptical galaxies

Details Clues on the hot star content and the ultraviolet output of elliptical galaxies Clues on the hot star content and the ultraviolet output of elliptical galaxies

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...364...35g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 364, Nov. 20, 1990, p. 35-64. Research supported by the Ministero dell'Univ

Mathematics

Logic

311

Elliptical Galaxies, Galactic Evolution, Hot Stars, Stellar Evolution, Ultraviolet Radiation, Asymptotic Giant Branch Stars, Binary Stars, Galactic Bulge, Metallicity, Stellar Luminosity, Stellar Models

Scientific paper

Purely energetic arguments are used here to investigate the conditions under which old, low-mass stars could be responsible for the UV rising branch of elliptical galaxies. It is argued that presently available observational data are insufficient to unambiguously decide which of various candidates provide the dominant contribution. It is found that the possibility for metal-rich, low-mass stars to evolve through sufficiently hot stages, provide enough UV photons, and produce the observed UV-metallicity correlation is primarily controlled by two poorly known trends with increasing metallicity: helium enrichment and mass-loss rate during the red giant phases. The classical hydrogen-burning post-AGB stars do not appear able to burn enough fuel to account for the most UV-powerful galaxies. Other hot star candidates which appear more promising are identified. It is shown that a very important role is played by the actual metallicity distribution within individual galaxies.

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