Caloric curves of classical self-gravitating systems in general relativity

Alberti, Giuseppe; Chavanis, Pierre‐Henri

doi:10.1103/physreve.101.052105

Cited by 18 publications

(91 citation statements)

References 174 publications

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“…The statistical mechanis of classical particles in general relativity has been considered by Roupas 55 and, independently, by Alberti and Chavanis. 1 The caloric curve depends on one parameter, the particle number N (more precisely N/R). Generically, the caloric curve β ∞ (E) has the form of a double spiral (see Fig.…”

Section: Classical Particles At T > 0 In General Relativitymentioning

confidence: 99%

“…h The hot spiral of ultrarelativistic classical particles in general relativity is similar, but not identical, to the hot spiral of the self-gravitating radiation. 1,3,54 become exact in a proper thermodynamic limit where N → +∞. This leads to the Fermi-Dirac-Poisson equations, also known as the temperature-dependent Thomas-Fermi equations.…”

Section: Nonrelativistic Fermions At T >mentioning

confidence: 99%

“…A more detailed historical account of the statistical mechanics and thermodynamics of self-gravitating systems (classical and quantum) in Newtonian gravity and general relativity can be found in Refs. [1][2][3][4] .…”

Section: Introductionmentioning

confidence: 99%

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The self-gravitating Fermi gas in Newtonian gravity and general relativity

Chavanis¹

2021

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We review the history of the self-gravitating Fermi gas in Newtonian gravity and general relativity. We mention applications to white dwarfs, neutron stars and dark matter halos. We describe the nature of instabilities and phase transitions in the self-gravitating Fermi gas as energy (microcanonical ensemble) or temperature (canonical ensemble) is reduced. When N < N OV , where N OV is the Oppenheimer-Volkoff critical particle number, the self-gravitating Fermi gas experiences a gravothermal catastrophe at Ec stopped by quantum mechanics (Pauli's exclusion principle). The equilibrium state has a core-halo structure made of a quantum core (degenerate fermion ball) surrounded by a classical isothermal halo. When N > N OV , a new turning point appears at an energy E c below which the system experiences a gravitational collapse towards a black hole [P.H. Chavanis, G. Alberti, Phys. Lett. B 801, 135155 (2020)]. When N OV < N < N * , the self-gravitating Fermi gas experiences a gravothermal catastrophe at Ec leading to a fermion ball, then a gravitational collapse at E c leading to a black hole. When N > N * , the condensed branch disappears and the instability at Ec directly leads to a black hole. We discuss implications of these results for dark matter halos made of massive neutrinos.

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Section: Classical Particles At T > 0 In General Relativitymentioning

confidence: 99%

Section: Nonrelativistic Fermions At T >mentioning

confidence: 99%

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The self-gravitating Fermi gas in Newtonian gravity and general relativity

Chavanis¹

2021

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“…It requires a relativistic approach analogous the one developed by Chavanis and Alberti in Refs. [41,[74][75][76], but including the incidence of evaporation effects. In general, one could expected many qualitative behaviors similar to the ones reported in Refs.…”

Section: The Kev Scale and The Masses Of Large Galaxiesmentioning

confidence: 99%

New Bounds for the Mass of Warm Dark Matter Particles Using Results from Fermionic King Model

Velázquez

2021

Universe

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After reviewing several aspects about the thermodynamics of self-gravitating systems that undergo the evaporation (escape) of their constituents, some recent results obtained in the framework of fermionic King model are applied here to the analysis of galactic halos considering warm dark matter (WDM) particles. According to the present approach, the reported structural parameters of dwarf galaxies are consistent with the existence of a WDM particle with mass in the keV scale. Assuming that the dwarf galaxy Willman 1 belongs to the region III of fermionic King model (whose gravothermal collapse is a continuous phase transition), one obtains the interval 1.2 keV ≤ m ≤ 2.6 keV for the mass of WDM particle. This analysis improves previous estimates by de Vega and co-workers [Astropart. Phys. 46 (2013) 14–22] considering both the quantum degeneration and the incidence of the constituents evaporation. This same analysis evidences that most of galaxies are massive enough to undergo a violent gravothermal collapse (a discontinuous microcanonical phase transition) that leads to the formation of a degenerate core of WDM particles. It is also suggested that quantum-relativistic processes governing the cores of large galaxies (e.g., the formation of supermassive black holes) are somehow related to the gravothermal collapse of the WDM degenerate cores when the total mass of these systems are comparable to the quantum-relativistic characteristic mass Mc=ℏc/G3/2m−2≃1012M⊙ obtained for WDM particles with mass m in the keV scale. The fact that a WDM particle with mass in the keV scale seems to be consistent with the observed properties of dwarf and large galaxies provides a strong support to this dark matter candidate.

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“…This expectation was shown to be correct in Refs. [11][12][13][14][15][16] for massive particle systems (see also [17,18] for radiation). They showed a curve for the series of equilibria has a double spiral structure.…”

Section: Introductionmentioning

confidence: 99%

Thermal equilibrium states and instability of self-gravitating particles in an asymptotically AdS spacetime

Asami,

Yoo

2021

Preprint

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We investigate the existence and the stability of spherically symmetric thermal equilibrium states of the self-gravitating many-particle system which satisfies the Einstein-Vlasov equations with a negative cosmological constant. While a thermal equilibrium state of the self-gravitating particle system cannot have a finite mass without an artificial wall in the asymptotically flat case, in the asymptotically AdS case, the total mass can be finite without any artificial wall due to the AdS potential barrier. In this case, the typical size of the system is characterized by the AdS radius. The equilibrium states can be parametrized by two independent parameters. Taking the total rest mass as the unit and fixing the AdS radius, we obtain the one-parameter family of equilibria which describes a curve in the parameter space spanned by the gravothermal energy and the temperature. Then we investigate the instability of the system based on the turning point method for each value of the AdS radius. We find that the curve typically has a double spiral structure as in the asymptotically flat case with an artificial wall. The possible value of the gravothermal energy is restricted to the finite region between the first turning points on the two respective spirals.

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Caloric curves of classical self-gravitating systems in general relativity

Cited by 18 publications

References 174 publications

The self-gravitating Fermi gas in Newtonian gravity and general relativity

The self-gravitating Fermi gas in Newtonian gravity and general relativity

New Bounds for the Mass of Warm Dark Matter Particles Using Results from Fermionic King Model

Thermal equilibrium states and instability of self-gravitating particles in an asymptotically AdS spacetime

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