Scaling behaviour of a scalar field model of dark matter halos
arXiv:astro-ph/0401575 · doi:10.1111/j.1365-2966.2004.07679.x
Abstract
Galactic dark matter is modelled by a scalar field. In particular, it is shown that an analytically solvable toy model with a non-linear self-interaction potential U(Phi) leads to dark halo models which have the form of quasi-isothermal spheres. We argue that these fit better the observed rotation curves of galaxies than the centrally cusped halos of standard cold dark matter. The scalar field model predicts a proportionality between the central densities of the dark halos and the inverse of their core radii. We test this prediction successfully against a set of rotation curves of low surface brightness galaxies and nearby bright galaxies.
arXiv comment4 pages, 2 figures, accepted to Mon. Not. R. Astron. Soc
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