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Titolo:
Kaon condensation in proto-neutron star matter - art. no. 035803
Autore:
Pons, JA; Reddy, S; Ellis, PJ; Prakash, M; Lattimer, JM;
Indirizzi:
SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA SUNY StonyBrook Stony Brook NY USA 11794 tron, Stony Brook, NY 11794 USA Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain Univ Valencia Burjassot Spain E-46100 Astrofis, E-46100 Burjassot, Spain Univ Washington, Inst Nucl Theory, Seattle, WA 98195 USA Univ Washington Seattle WA USA 98195 t Nucl Theory, Seattle, WA 98195 USA Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA Univ Minnesota Minneapolis MN USA 55455 Astron, Minneapolis, MN 55455 USA
Titolo Testata:
PHYSICAL REVIEW C
fascicolo: 3, volume: 6203, anno: 2000,
pagine: 5803 -
SICI:
0556-2813(200009)6203:3<5803:KCIPSM>2.0.ZU;2-K
Fonte:
ISI
Lingua:
ENG
Soggetto:
ASYMMETRIC NUCLEAR-MATTER; EQUATION; FLUCTUATIONS; EVOLUTION; PHASE;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
--discip_EC--
Citazioni:
45
Recensione:
Indirizzi per estratti:
Indirizzo: Pons, JA SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA SUNY Stony Brook Stony Brook NY USA 11794 ny Brook, NY 11794 USA
Citazione:
J.A. Pons et al., "Kaon condensation in proto-neutron star matter - art. no. 035803", PHYS REV C, 6203(3), 2000, pp. 5803

Abstract

We study the equation of state of kaon-condensed matter including the effects of temperature and trapped neutrinos. Several different field-theoretical models for the nucleon-nucleon and kaon-nucleon interactions are considered. It is found that the order of the phase transition to a kaon-condensedphase, and whether or not Gibbs' rules for phase equilibrium can be satisfied in the case of a first order transition, depend sensitively on the choice of the kaon-nucleon interaction. To avoid the anomalous high-density behavior of previous models for the kaon-nucleon interaction, a new functionalform is developed. For all interactions considered, a first order phase transition is possible only for magnitudes of the kaon-nucleus optical potential greater than or similar to 100 MeV. The main effect of finite temperature, for any value of the lepton fraction, is to mute the effects of a firstolder transition, so that the thermodynamics becomes similar to that of a second order transition. Above a critical temperature, found to be at least30-60 MeV depending upon the interaction, the first order transition disappears. The phase boundaries in baryon density versus lepton number and baryon density versus temperature planes are delineated, which is useful in understanding the outcomes of proto-neutron star simulations. We find that thethermal effects on the maximum gravitational mass of neutron stars are as important as the effects of trapped neutrinos, in contrast to previously studied cases in which the matter contained only nucleons or in which hyperons and/or quark matter were considered. Kaon-condensed equations of State permit the existence of metastable neutron stars, because the maximum mass ofan initially hot, lepton-rich proto-neutron star is greater than that of acold, deleptonized neutron star. The large thermal effects imply that a metastable proto-neutron star's collapse to a black hole could occur much later than in previously studied cases that allow metastable configurations.

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Documento generato il 02/12/20 alle ore 08:14:07