H I in early-type galaxies. II - Mass loss and galactic winds

Details H I in early-type galaxies. II - Mass loss and galactic winds H I in early-type galaxies. II - Mass loss and galactic winds

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...204..365f&link_type=abstract

Astrophysical Journal, vol. 204, Mar. 1, 1976, pt. 1, p. 365-375, 377, 378.

Astronomy and Astrophysics

Astrophysics

382

Cosmic Gases, Galactic Evolution, Hydrogen Clouds, Intergalactic Media, Astrophysics, Cosmology, Elliptical Galaxies, Mass Transfer, Radio Sources (Astronomy), Spiral Galaxies, Stellar Evolution, Stellar Winds, Supernovae

Scientific paper

Implications of the low upper limits to the neutral-hydrogen content observed in E and S0 galaxies are examined. Evidence for mass loss in these systems is reviewed, mass loss by dying stars in them is analyzed, and it is shown that the gas must either be hidden in some undetectable form or be completely removed from the interstellar medium. Several ways to conceal the gas are considered and found to fail on one or more grounds, indicating that a removal mechanism is likely. Possible candidates investigated for such a mechanism are efficient star formation, sweeping by nuclear explosions, and hot supernova-driven galactic winds. It is shown that the presence of galactic winds in ellipticals not only can explain the observed lack of hydrogen, but also is apparently in agreement with other observations, including the lack of reddening in early-type galaxies and the preferential association of RF activity with massive ellipticals. The possibility that hot winds may provide internal removal mechanisms in the bulges of disk galaxies is briefly discussed.

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