Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves
Abstract If dark matter is composed of massive bosons, a Bose–Einstein condensation process must have occurred during the cosmological evolution. Therefore galactic dark matter may be in a form of a condensate, characterized by a strong self-interaction. We consider the effects of rotation on the Bo...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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SpringerOpen
2018-04-01
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| Series: | European Physical Journal C: Particles and Fields |
| Online Access: | http://link.springer.com/article/10.1140/epjc/s10052-018-5835-8 |
| _version_ | 1828291809805074432 |
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| author | Xiaoyue Zhang Man Ho Chan Tiberiu Harko Shi-Dong Liang Chun Sing Leung |
| author_facet | Xiaoyue Zhang Man Ho Chan Tiberiu Harko Shi-Dong Liang Chun Sing Leung |
| author_sort | Xiaoyue Zhang |
| collection | DOAJ |
| description | Abstract If dark matter is composed of massive bosons, a Bose–Einstein condensation process must have occurred during the cosmological evolution. Therefore galactic dark matter may be in a form of a condensate, characterized by a strong self-interaction. We consider the effects of rotation on the Bose–Einstein condensate dark matter halos, and we investigate how rotation might influence their astrophysical properties. In order to describe the condensate we use the Gross–Pitaevskii equation, and the Thomas–Fermi approximation, which predicts a polytropic equation of state with polytropic index $$n=1$$ n=1 . By assuming a rigid body rotation for the halo, with the use of the hydrodynamic representation of the Gross–Pitaevskii equation we obtain the basic equation describing the density distribution of the rotating condensate. We obtain the general solutions for the condensed dark matter density, and we derive the general representations for the mass distribution, boundary (radius), potential energy, velocity dispersion, tangential velocity and for the logarithmic density and velocity slopes, respectively. Explicit expressions for the radius, mass, and tangential velocity are obtained in the first order of approximation, under the assumption of slow rotation. In order to compare our results with the observations we fit the theoretical expressions of the tangential velocity of massive test particles moving in rotating Bose–Einstein condensate dark halos with the data of 12 dwarf galaxies and the Milky Way, respectively. |
| first_indexed | 2024-04-13T10:58:18Z |
| format | Article |
| id | doaj.art-f7a17ab7c18a4d84873651cc440c1f2c |
| institution | Directory Open Access Journal |
| issn | 1434-6044 1434-6052 |
| language | English |
| last_indexed | 2024-04-13T10:58:18Z |
| publishDate | 2018-04-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | European Physical Journal C: Particles and Fields |
| spelling | doaj.art-f7a17ab7c18a4d84873651cc440c1f2c2022-12-22T02:49:28ZengSpringerOpenEuropean Physical Journal C: Particles and Fields1434-60441434-60522018-04-0178412010.1140/epjc/s10052-018-5835-8Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curvesXiaoyue Zhang0Man Ho Chan1Tiberiu Harko2Shi-Dong Liang3Chun Sing Leung4School of Physics and Yat Sen School, Sun Yat-sen UniversityDepartment of Science and Environmental Studies, The Education University of Hong KongDepartment of Physics, Babes-Bolyai UniversitySchool of Physics, State Key Laboratory of Optoelectronic Material and Technology, Guangdong Province Key Laboratory of Display Material and Technology, Sun Yat-Sen UniversityDepartment of Applied Mathematics, Hong Kong Polytechnic UniversityAbstract If dark matter is composed of massive bosons, a Bose–Einstein condensation process must have occurred during the cosmological evolution. Therefore galactic dark matter may be in a form of a condensate, characterized by a strong self-interaction. We consider the effects of rotation on the Bose–Einstein condensate dark matter halos, and we investigate how rotation might influence their astrophysical properties. In order to describe the condensate we use the Gross–Pitaevskii equation, and the Thomas–Fermi approximation, which predicts a polytropic equation of state with polytropic index $$n=1$$ n=1 . By assuming a rigid body rotation for the halo, with the use of the hydrodynamic representation of the Gross–Pitaevskii equation we obtain the basic equation describing the density distribution of the rotating condensate. We obtain the general solutions for the condensed dark matter density, and we derive the general representations for the mass distribution, boundary (radius), potential energy, velocity dispersion, tangential velocity and for the logarithmic density and velocity slopes, respectively. Explicit expressions for the radius, mass, and tangential velocity are obtained in the first order of approximation, under the assumption of slow rotation. In order to compare our results with the observations we fit the theoretical expressions of the tangential velocity of massive test particles moving in rotating Bose–Einstein condensate dark halos with the data of 12 dwarf galaxies and the Milky Way, respectively.http://link.springer.com/article/10.1140/epjc/s10052-018-5835-8 |
| spellingShingle | Xiaoyue Zhang Man Ho Chan Tiberiu Harko Shi-Dong Liang Chun Sing Leung Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves European Physical Journal C: Particles and Fields |
| title | Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves |
| title_full | Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves |
| title_fullStr | Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves |
| title_full_unstemmed | Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves |
| title_short | Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves |
| title_sort | slowly rotating bose einstein condensate galactic dark matter halos and their rotation curves |
| url | http://link.springer.com/article/10.1140/epjc/s10052-018-5835-8 |
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