Dynamical collapse of isothermal and adiabatic triaxial protogalaxies.

Details Dynamical collapse of isothermal and adiabatic triaxial protogalaxies. Dynamical collapse of isothermal and adiabatic triaxial protogalaxies.

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996kfnt...12...13b&link_type=abstract

Kinematika Fiz. Nebesn. Tel, Tom 12, No. 6, p. 13 - 26

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Protogalaxies: Hydrodynamics, Protogalaxies: Collapse

Scientific paper

This is the first in a series of papers on the 3D modelling of triaxial galaxies formation carried out by smoothed particle hydrodynamics method. The authors use the triaxial model for initial conditions of protogalaxies. The protogalaxy body is modelled by a triaxial ellipsoid with semiaxes A, B, and C. Initial velocity field is defined by initial angular velocity Ω0. The total angular momentum does not coincide with semiaxes. Therefore, the initial velocity field can be described by the formula: V0(x,y,z) = [Ω0×r]. In this paper the authors discuss a set of models of isothermal and adiabatic collapse for pure gas triaxial protogalaxies.

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