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arXiv:astro-ph/0011107 (astro-ph)
[Submitted on 4 Nov 2000 (v1), last revised 7 Dec 2000 (this version, v2)]

Title:Maximally incompressible neutron star matter

Authors:Timothy S. Olson
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Abstract: Relativistic kinetic theory, based on the Grad method of moments as developed by Israel and Stewart, is used to model viscous and thermal dissipation in neutron star matter and determine an upper limit on the maximum mass of neutron stars. In the context of kinetic theory, the equation of state must satisfy a set of constraints in order for the equilibrium states of the fluid to be thermodynamically stable and for perturbations from equilibrium to propagate causally via hyperbolic equations. Application of these constraints to neutron star matter restricts the stiffness of the most incompressible equation of state compatible with causality to be softer than the maximally incompressible equation of state that results from requiring the adiabatic sound speed to not exceed the speed of light. Using three equations of state based on experimental nucleon-nucleon scattering data and properties of light nuclei up to twice normal nuclear energy density, and the kinetic theory maximally incompressible equation of state at higher density, an upper limit on the maximum mass of neutron stars averaging 2.64 solar masses is derived.
Comments: 8 pages, 2 figures
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/0011107
  (or arXiv:astro-ph/0011107v2 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/0011107
Journal reference: Phys. Rev. C63 (2000) 015802
Related DOI: https://doi.org/10.1103/PhysRevC.63.015802

Submission history

From: Timothy S. Olson [view email]
[v1] Sat, 4 Nov 2000 23:22:08 UTC (116 KB)
[v2] Thu, 7 Dec 2000 20:54:31 UTC (116 KB)
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