Statistics – Computation
Scientific paper
Dec 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...153..157b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 153, no. 1, Dec. 1985, p. 157-162. DFG-supported research.
Statistics
Computation
5
Computational Astrophysics, Galactic Evolution, Star Formation, Elliptical Galaxies, Factor Analysis, Spiral Galaxies, Stellar Mass
Scientific paper
The authors postulate a star formation law dρs = αmρGβmσGγmdt (ρs = increment of stellar density during dt, ρG = density and σG = velocity dispersion of the gas; α, β, γ are constants to be determined). They obtain for elliptical galaxies κ = γ:(β-3/2) = 2.4±0.2. An assumed maximum contrast of the stellar mass fraction s of ellipticals of different rotational velocities leads to upper bounds for the absolute values of the exponents: β ≤ 2.1, γ ≤ 1.5. If the present velocity dispersions of the disks of spiral galaxies show preferentially the early values, nearly the same value of κ is obtained. Again, an assumed Δlg s = +1 from Sa to Irr galaxies - thought to be a lower limit for the end of the early phase - leads to lower limits β ≥ 1.8, γ ≥ 0.6. If instead the dispersions are the result of diffusion of the stellar orbits, β lies around 2.4. An integer combination within the allowed region is β = 2, γ = 1. This is plausible for a cloud collision picture of star formation.
Brosche Peter
Lentes F.-Th.
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