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Titolo:
COMPOSITION AND STRUCTURE OF PROTONEUTRON STARS
Autore:
PRAKASH M; BOMBACI I; PRAKASH M; ELLIS PJ; LATTIMER JM; KNORREN R;
Indirizzi:
SUNY STONY BROOK,DEPT PHYS STONY BROOK NY 11794 UNIV CALIF SANTA BARBARA,INST THEORET PHYS SANTA BARBARA CA 93106 UNIV MINNESOTA,SCH PHYS & ASTRON MINNEAPOLIS MN 55455 SUNY STONY BROOK,DEPT EARTH & SPACE SCI STONY BROOK NY 11794
Titolo Testata:
Physics reports
fascicolo: 1, volume: 280, anno: 1997,
pagine: 2 - 77
SICI:
0370-1573(1997)280:1<2:CASOPS>2.0.ZU;2-I
Fonte:
ISI
Lingua:
ENG
Soggetto:
RELATIVISTIC HARTREE APPROXIMATION; NUCLEAR-MATTER EQUATION; NEUTRON-STARS; KAON CONDENSATION; WEAK INTERACTION; QUARK MATTER; SUPERNOVA EXPLOSIONS; TRANSVERSE-MOMENTA; FIELD-THEORY; STATE;
Keywords:
NEUTRON STARS; NEUTRINOS; SUPERNOVAE;
Tipo documento:
Review
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
86
Recensione:
Indirizzi per estratti:
Citazione:
M. Prakash et al., "COMPOSITION AND STRUCTURE OF PROTONEUTRON STARS", Physics reports, 280(1), 1997, pp. 2-77

Abstract

We investigate the structure of neutron stars shortly after they are born, when the entropy per baryon is of order 1 or 2 and neutrinos aretrapped on dynamical timescales. We find that the structure depends more sensitively on the composition of the star than on its entropy, and that the number of trapped neutrinos play an important role in determining the composition. Since the structure is chiefly determined by the pressure of the strongly interacting constituents and the nature ofthe strong interactions is poorly understood at high density, we consider several models of dense matter, including matter with strangeness-rich hyperons, a kaon condensate and quark matter. In all cases, the thermal effects for an entropy per baryon of order 2 or less are smallwhen considering the maximum neutron star mass. Neutrino trapping, however, significantly changes the maximum mass due to the abundance of electrons. When matter is allowed to contain only nucleons and leptons, trapping decreases the maximum mass by an amount comparable to, but somewhat larger than, the increase due to finite entropy. When matter is allowed to contain strongly interacting negatively charged particles, in the form of strange baryons, a kaon condensate, or quarks, trapping instead results in an increase in the maximum mass, which adds to the effects of finite entropy. A net increase of order 0.2M. occurs. The presence of negatively-charged particles has two major implicationsfor the neutrino signature of gravitational collapse supernovae. First, the value of the maximum mass will decrease during the early evolution of a neutron star as it loses trapped neutrinos, so that if a black hole forms, it either does so immediately after the bounce (accretion being completed in a second or two) or it is delayed for a neutrino diffusion timescale of similar to 10 s. The latter case is most likelyif the maximum mass of the hot star with trapped neutrinos is near 1.5M.. In the absence of negatively-charged hadrons, black hole formation would be due to accretion and therefore is likely to occur only immediately after bounce. Second, the appearance of hadronic negative charges results in a general softening of the equation of state that may be observable in the neutrino luminosities and average energies. Further, these additional negative charges decrease the electron fraction and may be observed in the relative excess of electron neutrinos compared to other neutrinos.

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Documento generato il 26/11/20 alle ore 13:21:46