Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...100..124v&link_type=abstract
Astronomy and Astrophysics, vol. 100, no. 1, July 1981, p. 124-137. Research supported by the Nederlandse Organisatie voor Zuiv
Astronomy and Astrophysics
Astrophysics
36
Chemical Evolution, Galactic Evolution, Galactic Structure, Interstellar Gas, Stellar Evolution, Stellar Motions, Abundance, Gas Density, Gas Dynamics, Kinetic Energy, Metallic Stars, Star Formation Rate, Stellar Mass Accretion, Supernovae
Scientific paper
An accretion model for the kinematical and chemical evolution of the galactic disk in the solar neighborhood is presented which takes into account the detailed z structure of the disk. The evolution of the gas and stars in a cylinder perpendicular to the galactic plane is described in terms of a galactic disk built up by infalling gas which loses its turbulent energy on a free-fall time scale until it attains its presently observed velocity dispersion; an acceleration mechanism accounts for the observed increase of stellar velocity dispersion with age. The chemical evolution of the gas and stars is calculated in an instantaneous recycling approximation. The model satisfactorily reproduces the observed gravitational acceleration perpendicular to the galactic plane as well as the age dependence of stellar velocity dispersions and the vertical gradient of stellar metallicities. From considerations of the kinetic energy balance of the gas, with energy input due to supernova explosions and dissipation due to cloud-cloud collisions, it is concluded that an additional energy source, possibly large-scale fluctuations in galactic gravitational potential, is required to maintain a constant gas velocity dispersion if the star formation rate is proportional to gas density.
de Jong Teije
Vader Patricia J.
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