Bosons star at finite temperature

Latifah, Siti; Sulaksono, A.; Mart, T.

doi:10.1103/physrevd.90.127501

Cited by 32 publications

(47 citation statements)

References 40 publications

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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%

“…For example, although our results are formally only valid for zero-temperature bosonic condensates, finite temperature effects are expected to be negligible for bosonic masses much larger than the central temperature of the host star [48,49], such as bosonic fields with masses keV inside old neutron stars or white dwarfs. In fact, Refs.…”

Section: A Stars May Survive Dark Matter Capturementioning

confidence: 88%

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Interaction between bosonic dark matter and stars

et al. 2016

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We provide a detailed analysis of how bosonic dark matter "condensates" interact with compact stars, extending significantly the results of a recent Letter [1]. We focus on bosonic fields with mass mB, such as axions, axion-like candidates and hidden photons. Self-gravitating bosonic fields generically form "breathing" configurations, where both the spacetime geometry and the field oscillate, and can interact and cluster at the center of stars. We construct stellar configurations formed by a perfect fluid and a bosonic condensate, and which may describe the late stages of dark-matter accretion onto stars, in dark matter-rich environments. These composite stars oscillate at a frequency which is a multiple of f = 2.5 × 10 14 mBc 2 /eV Hz. Using perturbative analysis and Numerical Relativity techniques, we show that these stars are generically stable, and we provide criteria for instability. Our results also indicate that the growth of the dark matter core is halted close to the Chandrasekhar limit. We thus dispel a myth concerning dark matter accretion by stars: dark mater accretion does not necessarily lead to the destruction of the star, nor to collapse to a black hole. Finally, we argue that stars with long-lived bosonic cores may also develop in other theories with effective mass couplings, such as (massless) scalar-tensor theories.

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Section: Discussionmentioning

confidence: 78%

Section: Discussionmentioning

confidence: 93%

Section: A Stars May Survive Dark Matter Capturementioning

confidence: 88%

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Interaction between bosonic dark matter and stars

et al. 2016

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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%

Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves

et al. 2018

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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. 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 rotata

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“…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%

Thin accretion disks around cold Bose–Einstein condensate stars

Dǎnilǎ

Harkó

Kovács³

2015

Eur. Phys. J. C

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Due to their superfluid properties some compact astrophysical objects, like neutron or quark stars, may contain a significant part of their matter in the form of a BoseEinstein condensate (BEC). Observationally distinguishing between neutron/quark stars and BEC stars is a major challenge for this latter theoretical model. An observational possibility of indirectly distinguishing BEC stars from neutron/quark stars is through the study of the thin accretion disks around compact general relativistic objects. In the present paper, we perform a detailed comparative study of the electromagnetic and thermodynamic properties of the thin accretion disks around rapidly rotating BEC stars, neutron stars and quark stars, respectively. Due to the differences in the exterior geometry, the thermodynamic and electromagnetic properties of the disks (energy flux, temperature distribution, equilibrium radiation spectrum, and efficiency of energy conversion) are different for these classes of compact objects. Hence in this preliminary study we have pointed out some astrophysical signatures that may allow one to observationally discriminate between BEC stars and neutron/quark stars.

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Bosons star at finite temperature

Cited by 32 publications

References 40 publications

Interaction between bosonic dark matter and stars

Interaction between bosonic dark matter and stars

Slowly rotating Bose Einstein condensate galactic dark matter halos, and their rotation curves

Thin accretion disks around cold Bose–Einstein condensate stars

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