Nuclear constraints on the inner edge of neutron star crusts

Details Nuclear constraints on the inner edge of neutron star crusts Nuclear constraints on the inner edge of neutron star crusts

2009-09-30

arxiv.org/abs/0909.5494v1

Nucl.Phys.A834:664c-666c,2010

Physics

Nuclear Physics

Nuclear Theory

3 pages, 2 figures, contribution to the 10th International Conference on Nucleus-Nucleus Collisions (NN2009), Beijing, China,

Scientific paper

10.1016/j.nuclphysa.2010.01.118

We show that the widely used parabolic approximation to the Equation of State (EOS) of asymmetric nuclear matter leads systematically to significantly higher core-crust transition densities and pressures. Using an EOS for neutron-rich nuclear matter constrained by the isospin diffusion data from heavy-ion reactions in the same sub-saturation density range as the neutron star crust, the density and pressure at the inner edge separating the liquid core from the solid crust of neutron stars are determined to be 0.040 fm$^{-3}$ $\leq \rho_{t}\leq 0.065$ fm$^{-3}$ and 0.01 MeV/fm$^{3}$ $\leq P_{t}\leq 0.26$ MeV/fm$^{3}$, respectively. Implications of these constraints on the Vela pulsar are discussed.

Affiliated with

Also associated with

No associations

Rating

Nuclear constraints on the inner edge of neutron star crusts does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Nuclear constraints on the inner edge of neutron star crusts, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Nuclear constraints on the inner edge of neutron star crusts will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-588942