EPJ Web of Conferences
Volume 20, 2012Hadron Nuclear Physics 2011 (HNP2011) “Quarks in Hadrons, Nuclei, and Hadronic Matter”
|Number of page(s)||6|
|Section||Nuclei, Neutrino, Astrophysics, and Hypernuclei|
|Published online||10 February 2012|
Formation and Evolution of Neutron Star Binaries: Masses of Neutron Stars
Department of Physics, Pusan National University, Pusan 609-735, Korea
a e-mail: firstname.lastname@example.org
Neutron star (NS) is one of the most interesting astrophysical compact objects for hardronic physics. It is believed that the central density of NS can reach several times the normal nuclear matter density (ρ0). Hence, the inner part of NS is the ultimate testing place for the physics of dense matter. Recently, the mass of NS in a NS-white dwarf (WD) binary PSR J1614-2230 has been estimated to be 1.97 ± 0.04M๏ . Since this estimate is based on the observed Shapiro delay, it can give the lower limit of the maximum NS mass and rules out many soft equations of state. On the other hand, all the well-measured NS masses in NS-NS binaries are smaller than 1.5M๏. In this work, by introducing the supercritical accretion during the binary evolution, we propose a possibility of forming higher mass NS in NS-WD binaries. In this scenario, the lifetimes of NS and WD progenitors are significantly different, and NS in NS-WD binary can accrete > 0.5M๏ after NS formation during the giant phase of the progenitor of WD. On the other hand, for the binary system with NS and heavier (> 8M๏) giants, the first-born NS will accrete more from the companion and can collapse into black hole. The only way to avoid the supercritical accretion is that the initial masses of progenitors of NS binary should be very close so that they evolve almost at the same time and don’t have time to accrete after NS formation.
© Owned by the authors, published by EDP Sciences, 2012
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