Stability of BEC galactic dark matter halos

Guzmán, F. S.; Lora-Clavijo, F. D.; González-Avilés, J. J.; Rivera-Paleo, F. J.

doi:10.1088/1475-7516/2013/09/034

Cited by 49 publications

(45 citation statements)

References 24 publications

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“…More recently, this result was confirmed using a simple thermodynamic argument [22]. On the other hand, Guzman [23] found that the self-gravitating BEC halos described in [20] are unstable, and that furthermore, a relationship exists between the halo size and the BEC self-interaction parameter, which may be untenable (see also [24]). However, Toth [25] showed that these difficulties arise from the inappropriate application of the Thomas-Fermi approximation, and recommended the use of a different density profile as an approximate static solution.…”

Section: Arxiv:14127152v1 [Hep-ph] 22 Dec 2014mentioning

confidence: 81%

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Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

Madarassy

Toth

2015

Phys. Rev. D

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Using recently developed nonrelativistic numerical simulation code, we investigate the stability properties of compact astrophysical objects that may be formed due to the Bose-Einstein condensation of dark matter. Once the temperature of a boson gas is less than the critical temperature, a Bose-Einstein condensation process can always take place during the cosmic history of the universe. Due to dark matter accretion, a Bose-Einstein condensed core can also be formed inside massive astrophysical objects such as neutron stars or white dwarfs, for example.Numerically solving the Gross-Pitaevskii-Poisson system of coupled differential equations, we demonstrate, with longer simulation runs, that within the computational limits of the simulation the objects we investigate are stable. Physical properties of a self-gravitating Bose-Einstein condensate are examined both in non-rotating and rotating cases.

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Section: Arxiv:14127152v1 [Hep-ph] 22 Dec 2014mentioning

confidence: 81%

“…Is a Bose star stable? Guzmán et al argued [23] that it is not. However, the mass profiles [18] that they examined were constructed on the basis of the Thomas-Fermi approximation.…”

Section: B Numerical Stabilitymentioning

confidence: 99%

Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

Madarassy

Toth

2015

Phys. Rev. D

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“…Thus despite the sharp cut-off of the halo density, the BEC dark matter candidate is consistent with the rotation curve data of all types of galaxies [23]. The dynamics of rotating Bose Condensate galactic dark matter halos, made of an ultralight spinless bosons, and the impact of the halo rotation on the galactic rotation curves was analyzed in [24].…”

Section: Introductionmentioning

confidence: 59%

Gravitational collapse of Bose-Einstein condensate dark matter halos

Harkó

2014

Phys. Rev. D

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We study the mechanisms of the gravitational collapse of the Bose-Einstein condensate dark matter halos, described by the zero temperature time-dependent nonlinear Schrödinger equation (the Gross-Pitaevskii equation), with repulsive inter-particle interactions. By using a variational approach, and by choosing an appropriate trial wave function, we reformulate the Gross-Pitaevskii equation with spherical symmetry as Newton's equation of motion for a particle in an effective potential, which is determined by the zero point kinetic energy, the gravitational energy, and the particles interaction energy, respectively. The velocity of the condensate is proportional to the radial distance, with a time dependent proportionality function. The equation of motion of the collapsing dark matter condensate is studied by using both analytical and numerical methods. The collapse of the condensate ends with the formation of a stable configuration, corresponding to the minimum of the effective potential. The radius and the mass of the resulting dark matter object are obtained, as well as the collapse time of the condensate. The numerical values of these global astrophysical quantities, characterizing condensed dark matter systems, strongly depend on the two parameters describing the condensate, the mass of the dark matter particle, and of the scattering length, respectively. The stability of the condensate under small perturbations is also studied, and the oscillations frequency of the halo is obtained. Hence these results show that the gravitational collapse of the condensed dark matter halos can lead to the formation of stable astrophysical systems with both galactic and stellar sizes.

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“…therein. These models embody plausible features of cold dark matter, in some respects showing advantages, but they may also have their own difficulties such as e.g., the problem of (gravitational) collapse [48], or overestimated total mass of DM halos for dwarf galaxies [46]. This motivates researchers to explore other models that would be free of the weak points.…”

Section: Application For Modeling Dark Mattermentioning

confidence: 99%

Geometric Aspects and Some Uses of Deformed Models of Thermostatistics

Gavrilik

2018

Universe

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Abstract:We consider diverse deformed Bose gas models (DBGMs) focusing on distributions and correlations of any order, and also on deformed thermodynamics. For so-called µ-deformed Bose gas model (µ-DBGM), main thermodynamic aspects are treated: total number of particles, deformed partition function, etc. Using a geometric approach, we confirm the existence of critical behavior-Bose-like condensation; we find the critical temperature T (µ) c depending on µ so thatfor µ > 0. This fact and other advantages of µ-DBGM relative to the usual Bose gas, e.g., stronger effective inter-particle attraction (controlled by the parameter µ), allow us to consider the condensate in µ-DBGM as a candidate for modeling dark matter. As another, quite successful application we discuss the usage of the two-parameter (μ, q)-deformed BGM for effective description of the peculiar (non-Bose like) behavior of two-pion correlations observed in the STAR experiment at RHIC (Brookhaven). Herein, we point out the transparent role of the two deformation parametersμ and q as being responsible for compositeness and (effective account of) interactions of pions, respectively.

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Stability of BEC galactic dark matter halos

Cited by 49 publications

References 24 publications

Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

Gravitational collapse of Bose-Einstein condensate dark matter halos

Geometric Aspects and Some Uses of Deformed Models of Thermostatistics

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