Please use this identifier to cite or link to this item: http://hdl.handle.net/10397/78486
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dc.contributorDepartment of Applied Mathematicsen_US
dc.creatorZhang, XYen_US
dc.creatorChan, MHen_US
dc.creatorHarko, Ten_US
dc.creatorLiang, SDen_US
dc.creatorLeung, CSen_US
dc.date.accessioned2018-09-28T01:16:41Z-
dc.date.available2018-09-28T01:16:41Z-
dc.identifier.issn1434-6044en_US
dc.identifier.urihttp://hdl.handle.net/10397/78486-
dc.language.isoenen_US
dc.publisherSpringeren_US
dc.rights© The Author(s) 2018en_US
dc.rightsOpen Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. Funded by SCOAP3en_US
dc.rightsThe following publication Zhang, X., Chan, M. H., Harko, T., Liang, S. -., & Leung, C. S. (2018). Slowly rotating bose einstein condensate galactic dark matter halos, and their rotation curves. European Physical Journal C, 78(4), 346 is available at https://dx.doi.org/10.1140/epjc/s10052-018-5835-8en_US
dc.titleSlowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curvesen_US
dc.typeJournal/Magazine Articleen_US
dc.identifier.volume78en_US
dc.identifier.issue4en_US
dc.identifier.doi10.1140/epjc/s10052-018-5835-8en_US
dcterms.abstractIf 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. 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.en_US
dcterms.accessRightsopen accessen_US
dcterms.bibliographicCitationEuropean physical journal. C particles and fields, 28 Apr. 2018, v. 78, no. 4, 346en_US
dcterms.isPartOfEuropean physical journal. C, Particles and fieldsen_US
dcterms.issued2018-
dc.identifier.isiWOS:000432075200005-
dc.identifier.eissn1434-6052en_US
dc.identifier.artn346en_US
dc.identifier.rosgroupid2017006741-
dc.description.ros2017-2018 > Academic research: refereed > Publication in refereed journalen_US
dc.description.validate201809 bcrcen_US
dc.description.oaVersion of Recorden_US
dc.identifier.FolderNumberOA_IR/PIRAen_US
dc.description.pubStatusPublisheden_US
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