Intensity of gravitational waves emitted by pulsar neutron stars due to r-mode oscillation

The temperature T > 10¹¹K in newly born neutron stars (NSs) and the star enters the region of instability as it cools. In old cold NSs in a binary system, the star can enter the region of instability as it accretes mass from its companion. The r-mode amplitude α of a pulsar NS in the region of instability goes on increasing till a saturation is reached. At this point it emits a massive gravitational wave (GW) radiating energy and angular momentum and spins down to the region of stability. The spin-down rate can be calculated from the observed luminosity of the NS. The intensity of the emitted GW can be estimated from the amplitude of the GW strain tensor h₀