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Star formation and evolution in spiral galaxies.Evolutionary models for regions of M31 and M33 and the solar neighborhood are based on a stellar birthrate suggested by the dynamics of spiral structure: we assume that stars are formed very efficiently until the gas content reaches equilibrium at its present value, which takes about 1 b.y.; thereafter, the birthrate just equals the rate at which gas enters the system from stellar mass-loss or infall of intergalactic matter. Each model represents an average around a cylindrical-shell-shaped region, which is homogeneous and closed except for possible infall. The disk and spiral-arm populations only are considered. Each star is followed in the H-R diagram from the main sequence to death as an invisible remnant. Integrated magnitudes, colors, mass-to-light ratio (M/L), gas content, helium and metal abundance (Z), are computed in steps of 1 b.y.
Document ID
19730034253
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Quirk, W. J.
(NASA Goddard Institute for Space Studies New York, N.Y., United States)
Tinsley, B. M.
(Texas, University Dallas, Tex., United States)
Date Acquired
August 7, 2013
Publication Date
January 1, 1973
Publication Information
Publication: Astrophysical Journal
Volume: 179
Subject Category
Space Sciences
Accession Number
73A19055
Funding Number(s)
CONTRACT_GRANT: NSF GP-31413
CONTRACT_GRANT: NSF GP-23780
CONTRACT_GRANT: NSF GP-30455X
CONTRACT_GRANT: NSF GP-9527
Distribution Limits
Public
Copyright
Other

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