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Article: Could pressureless dark matter have pressure?

TitleCould pressureless dark matter have pressure?
Authors
KeywordsAnisotropic pressure
Barotropic equation
Constant velocities
Dark matter
Dark matter halos
Issue Date2012
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphys
Citation
Astroparticle Physics, 2012, v. 35 n. 9, p. 547-551 How to Cite?
AbstractA two-fluid dark matter model, in which dark matter is represented as a two-component fluid thermodynamic system, without interaction between the constituent particles of different species, and with each distinct component having a different four-velocity, was recently proposed in Harko and Lobo [T. Harko, F.S.N. Lobo, Phys. Rev. D 83 (2011) 124051]. In the present paper we further investigate the two-fluid dark matter model, by assuming that the two dark matter components are pressureless, non-comoving fluids. For this particular choice of equations of state the dark matter distribution can be described as a single anisotropic fluid, with vanishing tangential pressure, and non-zero radial pressure. We investigate the properties of this model in the region of constant velocity galactic rotation curves, where the dynamics of the test particles is essentially determined by the dark matter only. By solving the general relativistic equations of mass continuity and hydrostatic equilibrium we obtain the geometric and physical parameters of the dark matter halos in the constant velocity region in an exact analytical form. The general, radial coordinate dependent, functional relationship between the energy density and the radial pressure is also determined, and it differs from a simple barotropic equation of state. © 2012 Elsevier B.V. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/146901
ISSN
2015 Impact Factor: 3.425
2015 SCImago Journal Rankings: 1.612
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorHarko, Ten_US
dc.contributor.authorLobo, FSNen_US
dc.date.accessioned2012-05-23T05:49:04Z-
dc.date.available2012-05-23T05:49:04Z-
dc.date.issued2012en_US
dc.identifier.citationAstroparticle Physics, 2012, v. 35 n. 9, p. 547-551en_US
dc.identifier.issn0927-6505-
dc.identifier.urihttp://hdl.handle.net/10722/146901-
dc.description.abstractA two-fluid dark matter model, in which dark matter is represented as a two-component fluid thermodynamic system, without interaction between the constituent particles of different species, and with each distinct component having a different four-velocity, was recently proposed in Harko and Lobo [T. Harko, F.S.N. Lobo, Phys. Rev. D 83 (2011) 124051]. In the present paper we further investigate the two-fluid dark matter model, by assuming that the two dark matter components are pressureless, non-comoving fluids. For this particular choice of equations of state the dark matter distribution can be described as a single anisotropic fluid, with vanishing tangential pressure, and non-zero radial pressure. We investigate the properties of this model in the region of constant velocity galactic rotation curves, where the dynamics of the test particles is essentially determined by the dark matter only. By solving the general relativistic equations of mass continuity and hydrostatic equilibrium we obtain the geometric and physical parameters of the dark matter halos in the constant velocity region in an exact analytical form. The general, radial coordinate dependent, functional relationship between the energy density and the radial pressure is also determined, and it differs from a simple barotropic equation of state. © 2012 Elsevier B.V. All rights reserved.-
dc.languageengen_US
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphysen_US
dc.relation.ispartofAstroparticle Physicsen_US
dc.subjectAnisotropic pressure-
dc.subjectBarotropic equation-
dc.subjectConstant velocities-
dc.subjectDark matter-
dc.subjectDark matter halos-
dc.titleCould pressureless dark matter have pressure?en_US
dc.typeArticleen_US
dc.identifier.emailHarko, T: harko@hkucc.hku.hken_US
dc.identifier.emailLobo, FSN: flobo@cii.fc.ul.pt-
dc.identifier.authorityHarko, TC=rp01333en_US
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1016/j.astropartphys.2012.01.001-
dc.identifier.scopuseid_2-s2.0-84856410752-
dc.identifier.hkuros199783en_US
dc.identifier.volume35en_US
dc.identifier.issue9-
dc.identifier.spage547en_US
dc.identifier.epage551en_US
dc.identifier.isiWOS:000302109200001-
dc.publisher.placeNetherlandsen_US
dc.identifier.citeulike10228359-

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