Type II critical phenomena of neutron star collapse

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dc.creatorNoble, Scott C.
dc.creatorChoptuik, Matthew W.
dc.date2007-09-21
dc.date.accessioned2026-07-07T11:53:12Z
dc.date.available2026-07-07T11:53:12Z
dc.descriptionWe investigate spherically-symmetric, general relativistic systems of collapsing perfect fluid distributions. We consider neutron star models that are driven to collapse by the addition of an initially "in-going" velocity profile to the nominally static star solution. The neutron star models we use are Tolman-Oppenheimer-Volkoff solutions with an initially isentropic, gamma-law equation of state. The initial values of 1) the amplitude of the velocity profile, and 2) the central density of the star, span a parameter space, and we focus only on that region that gives rise to Type II critical behavior, wherein black holes of arbitrarily small mass can be formed. In contrast to previously published work, we find that--for a specific value of the adiabatic index (Gamma = 2)--the observed Type II critical solution has approximately the same scaling exponent as that calculated for an ultrarelativistic fluid of the same index. Further, we find that the critical solution computed using the ideal-gas equations of state asymptotes to the ultrarelativistic critical solution.
dc.description24 pages, 22 figures, RevTeX 4, submitted to Phys. Rev. D
dc.identifierhttps://arxiv.org/abs/0709.3527
dc.identifierhttp://arxiv.org/abs/0709.3527
dc.identifierPhys.Rev.D78:064059,2008
dc.identifierdoi:10.1103/PhysRevD.78.064059
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/204457
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleType II critical phenomena of neutron star collapse
dc.typetext

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