Speaker
Description
The observed spin frequency distribution of millisecond (ms) pulsars is a result of their current or previous spin evolution in the low-mass X-ray binary phase. Such a spin evolution depends on various physical aspects, such as binary evolution, disk-magnetosphere interaction, continuous gravitational wave emission, transient accretion, neutron star equations of state, etc. Thus, the computation of ms pulsar evolution, when performed considering these aspects, provides an excellent way to estimate the ellipticity of some pulsars and to prepare one to utilize the future continuous gravitational wave data from ms pulsars to probe the neutron star physics. Here, we will discuss the crucial effect of transient accretion on the spin evolution of ms pulsars, and how this effect indicates continuous gravitational wave emission from some pulsars. [Reference: (1) Bhattacharyya and Chakrabarty, 2017, ApJ, 835, 4; (2) Bhattacharyya, 2021, MNRAS, 502, L45].
