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(Φ) leads to dark halo models which have the form of quasi-isothermal spheres. We argue that these fit the observed rotation curves of galaxies better than the centrally cusped haloes of standard cold dark matter. The scalar field model predicts a proportionality between the central densities of the dark haloes 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.
Description
Scaling behaviour of a scalar field model of dark matter haloes - Fuchs - 2004 - Monthly Notices of the Royal Astronomical Society - Wiley Online Library
%0 Journal Article
%1 MNR:MNR7679
%A Fuchs, B.
%A Mielke, E. W.
%D 2004
%I Blackwell Science Ltd
%J Monthly Notices of the Royal Astronomical Society
%K dark_matter_halo solitons
%N 2
%P 707--709
%R 10.1111/j.1365-2966.2004.07679.x
%T Scaling behaviour of a scalar field model of dark matter haloes
%U http://dx.doi.org/10.1111/j.1365-2966.2004.07679.x
%V 350
%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(Φ) leads to dark halo models which have the form of quasi-isothermal spheres. We argue that these fit the observed rotation curves of galaxies better than the centrally cusped haloes of standard cold dark matter. The scalar field model predicts a proportionality between the central densities of the dark haloes 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.
@article{MNR:MNR7679,
abstract = {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(Φ) leads to dark halo models which have the form of quasi-isothermal spheres. We argue that these fit the observed rotation curves of galaxies better than the centrally cusped haloes of standard cold dark matter. The scalar field model predicts a proportionality between the central densities of the dark haloes 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.},
added-at = {2011-03-16T04:18:34.000+0100},
author = {Fuchs, B. and Mielke, E. W.},
biburl = {https://www.bibsonomy.org/bibtex/2e0476a4b13e70bfe65359e88badcb73d/casvada},
description = {Scaling behaviour of a scalar field model of dark matter haloes - Fuchs - 2004 - Monthly Notices of the Royal Astronomical Society - Wiley Online Library},
doi = {10.1111/j.1365-2966.2004.07679.x},
interhash = {7070a7526d49bb6991f066ccf73d3bec},
intrahash = {e0476a4b13e70bfe65359e88badcb73d},
issn = {1365-2966},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {dark_matter_halo solitons},
number = 2,
pages = {707--709},
publisher = {Blackwell Science Ltd},
timestamp = {2011-03-16T04:18:34.000+0100},
title = {Scaling behaviour of a scalar field model of dark matter haloes},
url = {http://dx.doi.org/10.1111/j.1365-2966.2004.07679.x},
volume = 350,
year = 2004
}