The evolution of flows of stellar mass loss in active galaxies

Details The evolution of flows of stellar mass loss in active galaxies The evolution of flows of stellar mass loss in active galaxies

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.197..995m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 197, Dec. 1981, p. 995-1019. Research supported by the Science Research

Computer Science

Numerical Analysis

99

Active Galaxies, Astronomical Models, Elliptical Galaxies, Flow Characteristics, Galactic Evolution, Gas Flow, Stellar Winds, Equations Of State, Galactic Radiation, Galactic Structure, Numerical Analysis, Stellar Evolution, Supernovae

Scientific paper

Gas flows in elliptical galaxies fuelled by stellar mass loss are calculated numerically for three fiducial epochs using both King and de Vaucouleurs models of NGC 3379. The results show that supernova heating is unable to prevent the inflow of stellar mass loss for a large proportion of the lifetime of most giant elliptical galaxies, irrespective of their detailed structure. The model presented explains the association of nuclear activity with giant elliptical galaxies and predicts rapid co-moving density evolution, as observed. The importance of considering the fate of stellar mass loss in elliptical galaxies is demonstrated.

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