Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves
We present a comparative confrontation of both the Bose-Einstein Condensate (BEC) and the Navarro-Frenk-White (NFW) dark halo models with galactic rotation curves. We employ 6 High Surface Brightness (HSB), 6 Low Surface Brightness (LSB), and 7 dwarf galaxies with rotation curves falling into two cl...
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doaj-8dfa571faae0490ab27eb4aab57abd692020-11-24T20:55:10ZengHindawi LimitedAdvances in High Energy Physics1687-73571687-73652017-01-01201710.1155/2017/40253864025386Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation CurvesM. Dwornik0Z. Keresztes1E. Kun2L. Á. Gergely3Institute of Physics, University of Szeged, Dóm Tér 9, Szeged 6720, HungaryInstitute of Physics, University of Szeged, Dóm Tér 9, Szeged 6720, HungaryInstitute of Physics, University of Szeged, Dóm Tér 9, Szeged 6720, HungaryInstitute of Physics, University of Szeged, Dóm Tér 9, Szeged 6720, HungaryWe present a comparative confrontation of both the Bose-Einstein Condensate (BEC) and the Navarro-Frenk-White (NFW) dark halo models with galactic rotation curves. We employ 6 High Surface Brightness (HSB), 6 Low Surface Brightness (LSB), and 7 dwarf galaxies with rotation curves falling into two classes. In the first class rotational velocities increase with radius over the observed range. The BEC and NFW models give comparable fits for HSB and LSB galaxies of this type, while for dwarf galaxies the fit is significantly better with the BEC model. In the second class the rotational velocity of HSB and LSB galaxies exhibits long flat plateaus, resulting in better fit with the NFW model for HSB galaxies and comparable fits for LSB galaxies. We conclude that due to its central density cusp avoidance the BEC model fits better dwarf galaxy dark matter distribution. Nevertheless it suffers from sharp cutoff in larger galaxies, where the NFW model performs better. The investigated galaxy sample obeys the Tully-Fisher relation, including the particular characteristics exhibited by dwarf galaxies. In both models the fitting enforces a relation between dark matter parameters: the characteristic density and the corresponding characteristic distance scale with an inverse power.http://dx.doi.org/10.1155/2017/4025386 |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
M. Dwornik Z. Keresztes E. Kun L. Á. Gergely |
spellingShingle |
M. Dwornik Z. Keresztes E. Kun L. Á. Gergely Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves Advances in High Energy Physics |
author_facet |
M. Dwornik Z. Keresztes E. Kun L. Á. Gergely |
author_sort |
M. Dwornik |
title |
Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves |
title_short |
Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves |
title_full |
Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves |
title_fullStr |
Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves |
title_full_unstemmed |
Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves |
title_sort |
bose-einstein condensate dark matter halos confronted with galactic rotation curves |
publisher |
Hindawi Limited |
series |
Advances in High Energy Physics |
issn |
1687-7357 1687-7365 |
publishDate |
2017-01-01 |
description |
We present a comparative confrontation of both the Bose-Einstein Condensate (BEC) and the Navarro-Frenk-White (NFW) dark halo models with galactic rotation curves. We employ 6 High Surface Brightness (HSB), 6 Low Surface Brightness (LSB), and 7 dwarf galaxies with rotation curves falling into two classes. In the first class rotational velocities increase with radius over the observed range. The BEC and NFW models give comparable fits for HSB and LSB galaxies of this type, while for dwarf galaxies the fit is significantly better with the BEC model. In the second class the rotational velocity of HSB and LSB galaxies exhibits long flat plateaus, resulting in better fit with the NFW model for HSB galaxies and comparable fits for LSB galaxies. We conclude that due to its central density cusp avoidance the BEC model fits better dwarf galaxy dark matter distribution. Nevertheless it suffers from sharp cutoff in larger galaxies, where the NFW model performs better. The investigated galaxy sample obeys the Tully-Fisher relation, including the particular characteristics exhibited by dwarf galaxies. In both models the fitting enforces a relation between dark matter parameters: the characteristic density and the corresponding characteristic distance scale with an inverse power. |
url |
http://dx.doi.org/10.1155/2017/4025386 |
work_keys_str_mv |
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1716792351365529600 |