Impact of accretion on the statistics of neutron star masses

We have collected the parameter of 38 neutron stars (NSs) in binary systems with spin periods and measured masses. By adopting the Boot-strap method, we reproduced the procedure of mass calculated for each system separately, to determine the truly mass distribution of the NS that obtained from observation. We also applied the Monte-Carlo simulation and introduce the characteristic spin period 20 ms, in order to distinguish between millisecond pulsars (MSPs) and less recycled pulsars. The mass distributions of MSPs and the less recycled pulsars could be fitted by a Gaussian function as $rm 1.45pm0.42 M_{odot}$ and $rm 1.31pm0.17 M_{odot} (rm with ~ 1sigma)$ respectively. As such, the MSP masses are heavier than those in less recycled systems by factor of $rm sim 0.13M_{odot}$, since the accretion effect during the recycling process.

Deriving fundamental parameters of millisecond pulsars via AIC in white dwarfs

We present a study of the observational properties of Millisecond Pulsars (MSPs) by way of their magnetic fields, spin periods and masses. These measurements are derived through the scenario of Accretion Induced Collapse (AIC) of white dwarfs (WDs) in stellar binary systems, in order to provide a greater understanding of the characteristics of MSP populations. In addition, we demonstrate a strong evolutionary connection between neutron stars and WDs with binary companions from a stellar binary evolution perspective via the AIC process.