Statistics – Computation
Scientific paper
May 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..241l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, May 20, 1990, p. 241-254.
Statistics
Computation
91
Neutron Stars, Pulsars, Stellar Models, Stellar Rotation, Computational Astrophysics, Equations Of State, Nuclear Astrophysics, Stellar Mass, Supernova 1987A
Scientific paper
It has recently been claimed that a submillisecond pulsar has been observed in the remnant of SN 1987A. If the pulsations are due to rotation of a neutron star at this frequency, the equation of state (EOS) must be severely limited. In general, soft equations of state allow rapid enough rotational frequencies, but the softness is limited by the observed neutron star mass of 1.44 solar mass in the binary pulsar PSR 1913 + 16. In order to simultaneously satisfy these two constraints, that, in the vicinity of ordinary nuclear density, the pressure must vary relatively slowly with density, but at higher densities, the EOS must become relatively stiff and approach the causality limit. Specifically, in the absence of phase transitions above nuclear density and for cases in which the nuclear symmetry energy is an increasing function of density, the compression modulus of symmetric nuclear matter at the saturation density 0.16/cu fm must be less than about 160 MeV. If either of these situations occurs, higher values for the compression modulus may be possible, but, in any case, the EOS must still stiffen to the causal limit at high density. Examples of phase transitions that might permit rapid enough rotation are those due to pion or kaon condensates or to parity-doublet matter occurring around a few times the nuclear matter density.
Lattimer James M.
Masak Dieter
Prakash Madappa
Yahil Amos
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