Gravitational phase transition of fermionic matter

Bilić, Neven; Viollier, Raoul D.

doi:10.1016/s0370-2693(97)00825-3

Cited by 75 publications

(86 citation statements)

References 21 publications

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“…The result of this phase transition is a "fermion ball" which contains almost all the mass (q 1) unlike in the microcanonical ensemble at the point of gravothermal catastrophe. These fermion balls can be of astrophysical interest in Dark Matter models consisting of massive neutrinos (Bilic & Viollier 1997;Chavanis 2002e). For rotating systems, the isothermal collapse is accompanied by a discontinuous rise of angular velocity at the critical temperature T c (see Fig.…”

Section: Rotating Self-gravitating Fermionsmentioning

confidence: 99%

Gravitational instability of slowly rotating isothermal spheres

Chavanis

2002

A&A

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Abstract. We discuss the statistical mechanics of rotating self-gravitating systems by allowing properly for the conservation of angular momentum. We study analytically the case of slowly rotating isothermal spheres by expanding the solutions of the Boltzmann-Poisson equation in a series of Legendre polynomials, adapting the procedure introduced by Chandrasekhar (1933) for distorted polytropes. We show how the classical spiral of Lynden-Bell & Wood (1967) in the temperature-energy plane is deformed by rotation. We find that gravitational instability occurs sooner in the microcanonical ensemble and later in the canonical ensemble. According to standard turning point arguments, the onset of the collapse coincides with the minimum energy or minimum temperature state in the series of equilibria. Interestingly, it happens to be close to the point of maximum flattening. We generalize the singular isothermal solution to the case of a slowly rotating configuration. We also consider slowly rotating configurations of the self-gravitating Fermi gas at non-zero temperature.

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Section: Rotating Self-gravitating Fermionsmentioning

confidence: 99%

Gravitational instability of slowly rotating isothermal spheres

Chavanis

2002

A&A

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“…This fact leads to the limits on the mass of DM particle (Tremaine & Gunn, 1979;Boyarsky et al, 2009). The previous analytical models of dark matter haloes as self-gravitating fermionic gas (Ruffini & Stella, 1983;Bilic & Viollier, 1997;Merafina & Alberti, 2014;Chavanis, Lemou, Mehats, 2015;Domcke & Urbano, 2015;Vega & Sanchez, 2016;Arguelles et al, 2016;Di Paolo, Nesti, Villante, 2017) require non-trivial assumptions about the temperature of dark matter and their distribution function. In this paper, we propose the method of calculating cored density distributions without such disadvantages.…”

Section: Introductionmentioning

confidence: 99%

Cores in Dark Matter Haloes With Anisotropic Osipkov-Merritt Distribution and Maximal Phase-Space Density

Rudakovskyi

2017

OAP

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ABSTRACT. This paper describes the developed model of dark matter cored density profiles. This model was recently proposed by Dmytro Iakubovskyi (Iakubovskyi & Rudakovskyi, in preparation). It has only one extra parameter -the maximal value f max of phase-space distribution function -that turn a cusped Navarro-Frenk-White density profile into a cored one. This paper focuses on the estimation of the influence of velocity anisotropy on the cored density profile by using the Osipkov-Merritt model. The density profiles of the typical dwarf-spheroidal galaxy for different masses of fermionic dark matter particle and different anisotropy parameters r a was calculated. It was obtained that the influence of velocity anisotropy on the cored density profile is small.

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“…Several papers were devoted to the non-relativistic degenerate fermionic dark matter with or wihtout barionic component (see for example [2,3,4,5,6,7]). Papers whose topic is some aspect of the relativistic behaviour of these systems are rare ( [8]).…”

Section: Introductionmentioning

confidence: 99%

Determination of the upper and lower bound of the mass limit of degenerate fermionic dark matter objects

Kupi

2008

Phys. Rev. D

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We give a gravitational upper limit for the mass of static degenerate fermionic dark matter objects. The treatment we use includes fully relativistic equations for describing the static solutions of these objects. We study the influence of the annihilation of the particles on this mass limit. We give the change of its value over the age of the Universe with annihilation cross sections relevant for such fermions constituting the dark matter. Our calculations take into account the possibility of Dirac as well Majorana spinors.PACS numbers: 95.30. Sf, 95.35.+d,

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Gravitational phase transition of fermionic matter

Cited by 75 publications

References 21 publications

Gravitational instability of slowly rotating isothermal spheres

Gravitational instability of slowly rotating isothermal spheres

Cores in Dark Matter Haloes With Anisotropic Osipkov-Merritt Distribution and Maximal Phase-Space Density

Determination of the upper and lower bound of the mass limit of degenerate fermionic dark matter objects

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