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Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter Once the temperature of a bosonic gas is smaller than the critical, density dependent, transition temperature, a Bose-Einstein condensation process can take place during the cosmological evolution of the Universe. Bose-Einstein condensates are very strong candidates for dark matter, since they can solve some major issues in observational astrophysics, like, for example, the galactic core/cusp problem. The presence of the dark matter condensates also drastically affects the cosmic history of the Universe. In the present paper we analyze the effects of the finite dark matter temperature on the cosmological evolution of the Bose-Einstein condensate dark matter systems. We formulate the basic equations describing the finite temperature condensate, representing a generalized Gross-Pitaevskii equation that takes into account the presence of the thermal cloud in thermodynamic equilibrium with the condensate. The temperature dependent equations of state of the thermal cloud and of the condensate are explicitly obtained in an analytical form. By assuming a flat Friedmann-Robertson-Walker geometry, the cosmological evolution of the finite temperature dark matter filled Universe is considered in detail in the framework of a two interacting fluid dark matter model, describing the transition from the initial thermal cloud to the low temperature condensate state. The dynamics of the cosmological parameters during the finite temperature dominated phase of the dark matter evolution are investigated in detail, and it is shown that the presence of the thermal excitations leads to an overall increase in the expansion rate of the Universe. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Physical Review D American Physical Society (APS)

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Physical Review D , Volume 85 (8) – Apr 15, 2012
13 pages

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References (18)

Publisher
American Physical Society (APS)
Copyright
Copyright © 2012 The American Physical Society
ISSN
1550-2368
DOI
10.1103/PhysRevD.85.084012
Publisher site
See Article on Publisher Site

Abstract

Once the temperature of a bosonic gas is smaller than the critical, density dependent, transition temperature, a Bose-Einstein condensation process can take place during the cosmological evolution of the Universe. Bose-Einstein condensates are very strong candidates for dark matter, since they can solve some major issues in observational astrophysics, like, for example, the galactic core/cusp problem. The presence of the dark matter condensates also drastically affects the cosmic history of the Universe. In the present paper we analyze the effects of the finite dark matter temperature on the cosmological evolution of the Bose-Einstein condensate dark matter systems. We formulate the basic equations describing the finite temperature condensate, representing a generalized Gross-Pitaevskii equation that takes into account the presence of the thermal cloud in thermodynamic equilibrium with the condensate. The temperature dependent equations of state of the thermal cloud and of the condensate are explicitly obtained in an analytical form. By assuming a flat Friedmann-Robertson-Walker geometry, the cosmological evolution of the finite temperature dark matter filled Universe is considered in detail in the framework of a two interacting fluid dark matter model, describing the transition from the initial thermal cloud to the low temperature condensate state. The dynamics of the cosmological parameters during the finite temperature dominated phase of the dark matter evolution are investigated in detail, and it is shown that the presence of the thermal excitations leads to an overall increase in the expansion rate of the Universe.

Journal

Physical Review DAmerican Physical Society (APS)

Published: Apr 15, 2012

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