Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001pabei..19s..84m&link_type=abstract
"Progress in Astronomy, Vol. 19, Supp., p. 84 - 97 (2001). In: Proceedings of the Fourth China-Germany Workshop on Cosmology "Co
Astronomy and Astrophysics
Astronomy
Spiral Galaxies, Tully-Fisher Relation
Scientific paper
We show that the Tully-Fisher relation observed for spiral galaxies can be explained in the current scenario of galaxy formation without invoking subtle assumptions, provided that galactic-sized dark haloes have low concentrations which do not change significantly with halo circular velocity. This conclusion does not depend significantly on whether haloes have cuspy or flat profiles in the inner region. In such a system, both the disk and the halo may contribute significantly to the maximum rotation of the disk, and the gravitational interaction between the disk and halo components leads to tight relation between disk mass and maximum rotation velocity. The model can therefore be tested by studying the Tully-Fisher zero points for galaxies with different disk mass-to-light ratios. With model parameters (such as the ratio between disk and halo mass, the specific angular momentum of disk material, disk formation time) chosen in plausible ranges, the model can well accommodate the zero-point, slope, and scatter of the observed Tully-Fisher relation, as well as the observed large range of disk surface densities and sizes. About half of the gravitational force at maximum rotation comes from the disk component for normal disks, while the disk contribution is lower for galaxies with lower surface density. The halo profile required by the Tully-Fisher relation is as concentrated as that required by the observed rotation curves of faint disks, but less concentrated than that given by current simulations of CDM models. We discuss the implication of such profiles for structure formation in the universe and for the properties of dark matter.
Mao Shude
Mo Hou-Jun
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