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Dissipational galaxy formation. I - Effects of gasdynamics
Katz, Neal; Gunn, James E.
AA(Princeton University Observatory, NJ; Steward Observatory, Tucson, AZ), AB(Princeton University Observatory, NJ)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 377, Aug. 20, 1991, p. 365-381. Research supported by Pittsburgh Supercomputing Center. (ApJ Homepage)
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NASA/STI Keywords:
Computational Astrophysics, Dark Matter, Galactic Evolution, Gas Dynamics, Gravitational Fields, Algorithms, Angular Momentum, Astronomical Models
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An attempt is made here to model galaxy formation using a new general-purpose code for evolving self-gravitating fluids in three dimensions. The gravitational forces are calculated using a hierarchical tree algorithm, while the gasdynamic properties are determined by smoothed particle hydrodynamics. The collapse of isolated constant density perturbations, initially in solid-body rotation and in Hubble flow with perturbations consisting of dark and baryonic matter in a 10 to 1 ratio, are simulated. Two-component systems consisting of a thin gaseous disks and dark matter halos are made which resemble spiral galaxies. The disks transfer more than 50 percent of their original angular momentum to the dark halos and form at an angle of about 30 deg to the rotation axis of the halos. The disks are warped and beyond about 5 kpc have flat rotation curves and exponential surface density profiles. The gas never heats to the virial temperature but remains at less than 30,000 K.

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