Thermal mass limit of neutron cores

Roupas, Zacharias

doi:10.1103/physrevd.91.023001

Cited by 15 publications

(22 citation statements)

References 47 publications

(97 reference statements)

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“…1 In this Letter, we report the results of our recent investigations concerning the statistical mechanics of selfgravitating fermions at finite temperature in the framework of general relativity. They complete the previous works of Bilic and Viollier [25,26] and Roupas [27][28][29]. The complete study being extremely rich, all the details are given in a series of exhaustive papers [30][31][32][33].…”

Section: Introductionmentioning

confidence: 99%

Gravitational phase transitions and instabilities of self-gravitating fermions in general relativity

Chavanis

Alberti

2020

Physics Letters B

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We discuss the occurrence of gravitational phase transitions and instabilities in a gas of selfgravitating fermions within the framework of general relativity. In the classical (nondegenerate) limit, the system undergoes a gravitational collapse at low energies E < Ec and low temperatures T < Tc. This is called "gravothermal catastrophe" in the microcanonical ensemble and "isothermal collapse" in the canonical ensemble. When quantum mechanics is taken into account and when the particle number is below the Oppenheimer-Volkoff limit (N < NOV), complete gravitational collapse is prevented by the Pauli exclusion principle. In that case, the Fermi gas undergoes a gravitational phase transition from a gaseous phase to a condensed phase. The condensed phase represents a compact object like a white dwarf, a neutron star, or a dark matter fermion ball. When N > NOV, there can be a subsequent gravitational collapse below a lower critical energy E < E c or a lower critical temperature T < T c leading presumably to the formation of a black hole. The evolution of the system is different in the microcanonical and canonical ensembles. In the microcanonical ensemble, the system takes a "core-halo" structure. The core consists in a compact quantum object or a black hole while the hot halo is expelled at large distances. This is reminiscent of the red giant structure of low-mass stars or the implosion-explosion of massive stars (supernova). In the canonical ensemble, the system collapses as a whole towards a compact object or a black hole. This is reminiscent of the implosion of supermassive stars (hypernova).PACS numbers: 04.40. Dg, 05.70.Fh, 95.30.Sf, 95.35.+d

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Section: Introductionmentioning

confidence: 99%

Gravitational phase transitions and instabilities of self-gravitating fermions in general relativity

Chavanis

Alberti

2020

Physics Letters B

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“…They determined this maximum mass M OV = 0.7M ⊙ for ideal neutron cores. Roupas [30] generalized to all temperatures the original calculation of Oppenheimer & Volkoff, providing the analogue of Oppenheimer-Volkoff analysis for the whole cooling stage of a neutron star; from the ultra hot progenitor, the proto-neutron star [31][32][33], down to the final cold star. Bilic and Viollier [34], earlier, had studied the statistical mechanics of selfgravitating fermions in general relativity confined in a box.…”

Section: Introductionmentioning

confidence: 99%

Relativistic gravitational phase transitions and instabilities of the Fermi gas

Roupas¹,

Chavanis²

2019

Class. Quantum Grav.

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We describe microcanonical phase transitions and instabilities of the ideal Fermi gas in general relativity at nonzero temperature confined in the interior of a spherical shell. The thermodynamic behaviour is governed by the compactness of rest mass, namely of the total rest mass over radius of the system. For a fixed value of rest mass compactness, we study the caloric curves as a function of the size of the spherical box. At low compactness values, low energies and for sufficiently big systems the system is subject to a gravothermal catastrophe, which cannot be halted by quantum degeneracy pressure, and the system collapses. For small systems, there appears no instability at low energies. For intermediate sizes, between two marginal values, gravothermal catastrophe is halted and a microcanonical phase transition occurs from a gaseous phase to a condensed phase with a nearly degenerate core. The system is subject to a relativistic instability at low energy, when the core gets sufficiently condensed above the Oppenheimer-Volkoff limit. For sufficiently high values of rest mass compactness the microcanonical phase transitions are suppressed. They are replaced either by an Antonov type gravothermal catastrophe for sufficiently big systems or by stable equilibria for small systems. At high energies the system is subject to the 'relativistic gravothermal instability', identified by Roupas in [1], for all values of compactness and any size. ‡ This caloric curve was first plotted (by hand) by Katz [6]. § This notion of ensemble inequivalence for systems with long-range interactions is now well-known (see, e.g., [8]). This is to be contrasted to the case of systems with short-range interactions for which the statistical ensembles are equivalent in the thermodynamic limit [9].

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“…In this section we want to show how this effect manifest itself in thermal equilibrium ideal gases (isothermal spheres, in spherical, bounded, static configurations), and in neutron stars. To this goal, we will follow [16,18].…”

Section: Tolman-ehrenfest Law In Ideal Gases and Neutron Starsmentioning

confidence: 99%

“…A further generalization to arbitrary perfect fluids was also given by Gao [13,14]. Some time after, Roupas [15][16][17][18] specified in which thermodynamic ensemble the calculation must be performed thereby recalculating the TOV, TE, and Klein result. It is also worth mentioning that Rovelli and Smerlek [19] also obtained the TE relation by applying the equivalence principle to a property of thermal time.…”

Section: Introductionmentioning

confidence: 99%

Thermodynamic equilibrium in general relativity

2019

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The thermodynamic equilibrium condition for a static self-gravitating fluid in the Einstein theory is defined by the Tolman-Ehrenfest temperature law, T g 00 (x i ) = constant, according to which the proper temperature depends explicitly on the position within the medium through the metric coefficient g 00 (x i ). By assuming the validity of Tolman-Ehrenfest "pocket temperature", Klein also proved a similar relation for the chemical potential, namely, µ g 00 (x i ) = constant. In this letter we prove that a more general relation uniting both quantities holds regardless of the equation of state satisfied by the medium, and that the original Tolman-Ehrenfest law form is valid only if the chemical potential vanishes identically. In the general case of equilibrium, the temperature and the chemical potential are intertwined in such a way that only a definite (position dependent) relation uniting both quantities is obeyed. As an illustration of these results, the temperature expressions for an isothermal gas (finite spherical distribution) and a neutron star are also determined.

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Thermal mass limit of neutron cores

Cited by 15 publications

References 47 publications

Gravitational phase transitions and instabilities of self-gravitating fermions in general relativity

Gravitational phase transitions and instabilities of self-gravitating fermions in general relativity

Relativistic gravitational phase transitions and instabilities of the Fermi gas

Thermodynamic equilibrium in general relativity

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