Rotation curves from baryonic infall - Dependence on disk-to-halo ratio, initial angular momentum, and core radius, and comparison with data

Details Rotation curves from baryonic infall - Dependence on disk-to-halo ratio, initial angular momentum, and core radius, and comparison with data Rotation curves from baryonic infall - Dependence on disk-to-halo ratio, initial angular momentum, and core radius, and comparison with data

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..443f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 2, p. 443-454.

Other

106

Angular Momentum, Baryons, Dark Matter, Elementary Particles, Galactic Halos, Particle Mass, Adiabatic Conditions, Astronomical Models, Galactic Evolution, Rotating Matter

Scientific paper

A simple analytic mode of the response of dark matter halos to the dissipative infall of the luminous material to form an exponential disk is used to explore the dependence of the final rotation curves on all the relevant parameters: the ratio of the dissipative baryonic mass to the total galaxy mass, including dark matter; the ratio of the disk exponential scale length to the truncation radius; the core radius of the isothermal halo in the absence of dissipation; and the dimensionless angular momentum parameter. Particular attention is given to the final rotation curves expected in the tidal torque theory of angular momentum, in which (lambda) is about 0.05. For F of about 0.05 the dispersion in lambda expected in the tidal torque theory, 0.02-0.1, leads to rotation curves for bright galaxies whose systematics are much like those of galaxies for which H I data are available when consistent baryonic disk-scale lengths are used throughout. The mass inside R(H) exhibits a spread of values consistent with observations except possibly for the smallest galaxies, which may have suffered significant loss.

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