Locating the inner edge of the neutron star crust using terrestrial nuclear laboratory data
- Institute of Theoretical Physics, Shanghai Jiao Tong University, Shanghai 200240 (China)
- Department of Physics, Texas A and M University-Commerce, Commerce, Texas 75429-3011 (United States)
Within both dynamical and thermodynamical approaches using the equation of state for neutron-rich nuclear matter constrained by the recent isospin diffusion data from heavy-ion reactions in the same subsaturation 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{sup -3}{<=}{rho}{sub t}{<=}0.065 fm{sup -3} and 0.01 MeV/fm{sup 3}{<=}P{sub t}{<=}0.26 MeV/fm{sup 3}, respectively. These together with the observed minimum crustal fraction of the total moment of inertia allow us to set a new limit for the radius of the Vela pulsar significantly different from the previous estimate. It is further shown that the widely used parabolic approximation to the equation of state of asymmetric nuclear matter leads systematically to significantly higher core-crust transition densities and pressures, especially with stiffer symmetry energy functionals.
- OSTI ID:
- 21199641
- Journal Information:
- Physical Review. C, Nuclear Physics, Vol. 79, Issue 3; Other Information: DOI: 10.1103/PhysRevC.79.035802; (c) 2009 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); ISSN 0556-2813
- Country of Publication:
- United States
- Language:
- English
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