Physics – Nuclear Physics – Nuclear Theory
Scientific paper
2011-11-20
Physics
Nuclear Physics
Nuclear Theory
5 pages including 5 figures; Accepted for presentation at DAE Symposium on Nuclear Physics, December 26-30, 2011, Department o
Scientific paper
A nuclear equation of state (EoS) for $\beta$-equilibrated charge neutral neutron star (NS) matter was determined using density dependent effective nucleon-nucleon interaction which satisfies both the constraints from the observed mass-radius of neutron stars and flow data from heavy-ion collisions. Recent observations of the binary millisecond pulsar J1614-2230 by P. B. Demorest et al. \cite{De10} suggest that the masses lie within 1.97$\pm$0.04 M$_\odot$ where M$_\odot$ is the solar mass. Most EoS involving exotic matter, such as kaon condensates or hyperons, tend to predict maximum masses well below 2.0 M$_\odot$ and are therefore ruled out. Pure nucleonic EoS determines that the maximum mass of NS rotating with frequency below r-mode instability is $\sim$1.95 M$_\odot$ with radius $\sim$10 kilometers. At high densities the energy density of quark matter is lower than that of this nuclear EoS implying the possibility of deconfinement transition to quark matter inside. We find that the nuclear to quark matter transition inside neutron star cores causes reduction in their masses. Although in conformity with recent observations, such compact stars rotating with Kepler's frequency have masses up to $\sim$2 M$_\odot$, the compact stars rotating with maximum frequency limited by the r-mode instability, the maximum mass $\sim$1.72 M$_\odot$ turns out to be lower than the observed upper limit.
Basu D. N.
Chowdhury Partha Roy
Mishra Abhishek
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