Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....72..204d&link_type=abstract
Astronomy and Astrophysics, vol. 72, no. 1-2, Feb. 1979, p. 204-210.
Astronomy and Astrophysics
Astrophysics
4
Astronomical Models, Galactic Evolution, Galactic Rotation, Star Formation, Star Formation Rate, Boundary Value Problems, Density Distribution, Gravitational Effects, Interstellar Gas
Scientific paper
It is shown that initial conditions (i.e., the initial rotational and thermal parameters) affect the star-formation rate and determine whether a protogalaxy will evolve into a dissipation-damped disk or a nondissipatively relaxed spheroid. A protogalaxy is modeled as a Maclurin spheroid, the appropriate dynamical equations are integrated, and a phenomenological law describing star formation is adopted. This law is checked qualitatively by computing the growth of density perturbations, due to gravitational instabilities, up to the end of the linear regime. The results indicate that: (1) for low initial rotational and thermal energies, a high rate of star formation is attained, and an elliptical galaxy is formed nondissipatively; (2) in the opposite case the star-formation rate is low, a large amount of gas is left after one collapse time, and a dislike spiral galaxy is formed via dissipative mechanisms; and (3) S0 galaxies can be regarded as intermediate cases in the sense that the removal of gas, due to the star-formation process, occurs only after disk formation and metal enrichment.
di Fazio A.
Occhionero Franco
Vagnetti Fausto
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