Physics – Nuclear Physics – Nuclear Theory
Scientific paper
2010-02-09
Phys.Rev.C81:062801,2010
Physics
Nuclear Physics
Nuclear Theory
5 pages, 4 figures
Scientific paper
10.1103/PhysRevC.81.062801
Pure hadronic compact stars, above a limiting value ($\approx$1.6 M$_\odot$) of their gravitational masses, to which predictions of most of other equations of state (EoSs) are restricted, can be reached from the equation of state (EoS) obtained using DDM3Y effective interaction. This effective interaction is found to be quite successful in providing unified description of elastic and inelastic scattering, various radioactivities and nuclear matter properties. We present a systematic study of the properties of pure hadronic compact stars. The $\beta$-equilibrated neutron star matter using this EoS with a thin crust is able to describe highly-massive compact stars, such as PSR B1516+02B with a mass M=1.94$^{+0.17}_{-0.19}$ M$_\odot$ and PSR J0751+1807 with a mass M=2.1$\pm$0.2 M$_\odot$ to a 1$\sigma$ confidence level.
Basu D. N.
Bhattacharyya Abhijit
Chowdhury Partha Roy
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