Anisotropic models of galactic evolution

Details Anisotropic models of galactic evolution Anisotropic models of galactic evolution

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...199..131b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 199, no. 1-2, June 1988, p. 131-145.

Astronomy and Astrophysics

Astrophysics

34

Astronomical Models, Galactic Evolution, Galactic Structure, Interstellar Gas, Stellar Evolution, Elliptical Galaxies, Finite Difference Theory, Kinetic Energy, Legendre Functions, Navier-Stokes Equation, Poisson Equation

Scientific paper

The axisymmetric collapse of rotating protogalaxies is studied numerically applying the hydrodynamical Eulerian equation for the gaseous component and a generalized, anisotropic continuum model for the stellar system. The gas is assumed to be in a nonuniform turbulent state and dissipates its kinetic energy by cloud-cloud collisions. Stars form from the gas with an isotropic or anisotropic velocity dispersion and return metal-enriched gas to the ISM using a local instantaneous recycling approximation. The results show that this simple anisotropic hydrodynamical model of galactic evolution can explain at least the formation of two different components of galaxies: a spheroidal metal-poor halo and a rotationally supported metal-rich disk. However, no bulge is formed in the model. The models show a strong correlation between disk size and initial spin parameter lambda, suggesting that elliptical galaxies might form from protogalaxies with small lambda, whereas spiral galaxies would result from large lambda.

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