Speaker
Description
Numerical modeling of accreting millisecond X-ray pulsars (AMXPs) allows us to understand the physical origin of different observational signatures detected from these systems. Since the birth sites of these signals are strongly affected by the gravitational potential of the star, magnetohydrodynamic (MHD) simulations in full GR (GRMHD) are essential to accurately capture space-time curvature effects and inherent variations in the X-ray spectra. In this talk, I will be showing results from 3D GRMHD simulations of accreting neutron stars with oblique magnetospheres. I will be discussing the pulse profiles generated from the GRMHD simulations and their impact on M-R inference for the accreting sources. Apart from the surface features, AMXPs are also good candidates for studying neutron star jet formation. Though there have been extensive investigations into black hole jet formation, neutron star jets remain highly unexplored. Our 2D axisymmetric study in the quiescent regime suggests that the thick disk collimates the initial open stellar flux, leading to jets like the Blandford-Znajek mechanism proposed for black holes. However, much remains to be done before we can draw a complete picture of jets launched from neutron stars. 3D GRMHD simulations of accreting neutron stars allow us to explore neutron star jet formation mechanisms in detail for the very first time.
