Luminosity of M giants in the nuclear bulge of the Galaxy

Details Luminosity of M giants in the nuclear bulge of the Galaxy Luminosity of M giants in the nuclear bulge of the Galaxy

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259l...7f&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 259, Aug. 1, 1982, p. L7-L11.

Astronomy and Astrophysics

Astrophysics

47

Galactic Bulge, Giant Stars, M Stars, Milky Way Galaxy, Stellar Evolution, Stellar Luminosity, Asymptotic Giant Branch Stars, Galactic Nuclei, Spectral Energy Distribution, Stellar Color

Scientific paper

A color-luminosity diagram for 20 galactic bulge giants around NGC 6522 shows that Blanco types M7-M9 are on the upper asymptotic giant branch at a bolometric magnitude of -4.5, significantly fainter than the giant luminosities adopted in the Tinsley-Gunn galaxy population model but certainly more luminous than the He core flash luminosity assumed to be the upper limit in the models of Aaronson, Cohen, Mould, and Malkan. Distorted energy distributions and nonstandard colors relative to solar neighborhood M giants are attributed to a super-metal-rich (SMR) composition as is observed in bulge K giants by Whitford and Rich. Long main-sequence lifetimes for such SMR stars imply that those of initial mass ranging from 0.95 to 1.15 do not become giants until after 12-billion years. The additional mass over the usual initial mass of 0.8 for a metal-poor globular cluster star of the same age could be sufficient to fuel ascent onto the upper asymptotic branch, although it is still possible that some of the bulge giants are luminous because they are massive and young.

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