Galactic evolution. II - Disk galaxies with massive halos

Details Galactic evolution. II - Disk galaxies with massive halos Galactic evolution. II - Disk galaxies with massive halos

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202..353o&link_type=abstract

Astrophysical Journal, vol. 202, Dec. 1, 1975, pt. 1, p. 353-364.

Astronomy and Astrophysics

Astronomy

152

Galactic Evolution, Galactic Structure, Halos, Star Distribution, Stellar Evolution, Astronomical Models, Elliptical Galaxies, Galactic Radiation, Mathematical Models, Radio Astronomy, Spiral Galaxies, Stellar Mass

Scientific paper

Models of galactic evolution are computed in which matter shed by dying halo stars accumulates in a smaller, more rapidly rotating disk. The models are simpler and more successful than one-zone (pure disk) models in that (1) the observed absence of low-metal-abundance low-mass dwarfs is expected, not anomalous and (2) the relative birthrate function (or IMF) need not be a strongly variable function of time in agreement with recent interpretations of observed stellar populations and neutral hydrogen in our own and other galaxies. Even a simple 'Salpeter' IMF for both disk and halo will produce an acceptable model. The model with a halo 'Salpeter' IMF, roughly one-quarter of the mass in the secondary disk, and approximately half the metals produced in the halo seems most compatible with observations of the metal abundance in low-mass stars, the deuterium abundance, halo planetary nebulae, and light from Population II stars, as well as with arguments on the stability of the disk.

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