2014
DOI: 10.1103/physrevd.90.127501
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Bosons star at finite temperature

Abstract: By using a simple thermodynamical method we confirm the finding of Chavanis and Harko that stable Bose-Einstein condensate stars can form. However, by using a thermodynamically consistent boson equation of state, we obtain a less massive Bose-Einstein condensate star compared to the one predicted by Chavanis and Harko. We also obtain that the maximum mass of a boson star is insensitive to the change of matter temperature. However, the mass of boson star with relatively large radius depends significantly on the… Show more

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Cited by 32 publications
(47 citation statements)
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“…On the other hand, although more detailed studies of these effects are still necessary, the results of Refs. [48,49] suggest that, for bosonic fields with masses keV inside old neutron stars or white dwarfs, local thermalization should not significantly affect our results.…”
Section: Discussionmentioning
confidence: 78%
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“…On the other hand, although more detailed studies of these effects are still necessary, the results of Refs. [48,49] suggest that, for bosonic fields with masses keV inside old neutron stars or white dwarfs, local thermalization should not significantly affect our results.…”
Section: Discussionmentioning
confidence: 78%
“…As such, we expect that viscosity will damp global oscillations of the star, eventually leading to a depletion of the scalar field core. A similar effect will occur with local thermalization of the scalar with the star material if the central temperature of the star is much larger than the mass of the bosonic field [48,49]. On the other hand, although more detailed studies of these effects are still necessary, the results of Refs.…”
Section: Discussionmentioning
confidence: 93%
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“…Bose-Einstein condensate stars could have maximum masses of the order of 2 M , maximum central densities of the order of 0.1-0.3 ×10 16 g/cm 3 , and minimum radii in the range of 10-20 km, respectively. Their interesting physical and astrophysical properties were investigated in [63][64][65][66][67][68][69][70][71][72].…”
Section: Introductionmentioning
confidence: 99%
“…It was also suggested that the recently observed neutron stars with masses in the range of 2-2.4M (Vela X-1, 4U 1700-377, and the black widow pulsar B1957+20) are BEC stars. Further properties of BEC stars have been considered in [81][82][83][84].…”
Section: Introductionmentioning
confidence: 99%