Abstract
We perform MHD simulations of a thin resistive and viscous accretion disk around a neutron star with the surface dipolar magnetic field of 108 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.
Highlights
In the interaction of a neutron star (NS) with its close companion star, an accretion disk is formed around the NS
We show a zoom into this solution to show the accretion column and magnetospheric region in more detail
Most of the mass from the disk is accreted onto the star and only about 1/100 of it goes into the stellar wind
Summary
In the interaction of a neutron star (NS) with its close companion star, an accretion disk is formed around the NS. Kluzniak & Kita suggested a hydro-dynamical model for the accretion disk [1], with viscosity parameterized by Shakura & Sunyaev α-prescription [2]. We extend this model to the non-ideal MHD, and include the magnetosphere in the innermost part of a star-disk system. One example of such object is a millisecond pulsar: M = 1.4M⊙, R ∼ 10 km, B ∼ 108 Gauss, P = 0.05 sec (5 msec), ρ0 = 4.62 × 10−6 g/cm, M 0 = 10−9M⊙/yr
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