Equation of state and neutron star properties constrained by nuclear physics and observation. (arXiv:1303.4662v1 [astro-ph.SR]):
Microscopic calculations of neutron matter based on nuclear interactions
derived from chiral effective field theory, combined with the recent
observation of a 1.97 +- 0.04 M_sun neutron star, constrain the equation of
state of neutron-rich matter at sub- and supranuclear densities. We discuss in
detail the allowed equations of state and the impact of our results on the
structure of neutron stars, the crust-core transition density, and the nuclear
symmetry energy. In particular, we show that the predicted range for neutron
star radii is robust. For use in astrophysical simulations, we provide detailed
numerical tables for a representative set of equations of state consistent with
these constraints.
No comments:
Post a Comment