MHD simulations of resistive viscous accretion disk around millisecond pulsar

TL;DR

This paper presents magnetohydrodynamic simulations of a resistive, viscous accretion disk around a millisecond pulsar, revealing stable accretion and wind propagation over 500 pulsar rotations.

Contribution

It introduces detailed MHD simulations of a resistive viscous accretion disk around a millisecond pulsar, highlighting the system's evolution and stable accretion behavior.

Findings

Stable accretion column formation

Propagation of stellar wind through corona

Disk reaches quasi-stationary state

Abstract

We perform MHD simulations of a thin resistive and viscous accretion disk around a neutron star with the surface dipolar magnetic field of 10$^8$ Gauss. The system evolution is followed during the interval of 500 millisecond pulsar rotations. Matter is accreted through a stable accretion column from the disk onto the star. We also show propagation of the stellar wind through the corona. Analysis of the mass accretion flux and torques on the star shows that the disk reaches the quasi-stationary state.