R-Mode Instability of Neutron Stars Using Nuclear EoS from DDM3Y

Abstract

The r-mode instability windows and the gravitational wave signatures of neutron stars have been studied using $\beta$-equilibrated neutron-proton-electron neutron star matter at the core with a rigid crust. The fiducial gravitational and viscous timescales, the critical frequencies and the time evolutions of the frequencies and the rates of frequency change are calculated for a range of neutron star masses. It is found that the young and hot rotating massive neutron stars (NSs) are more susceptible to r-mode instability through gravitational radiation. We also find that NS for equation of state (EoS) with low L value lie in the r-mode instability region.