Many of the X-ray stars in low-mass binary systems are thought to be weakly magnetic neutron stars accreting from Keplerian disks. If the stellar magnetic field is ∼108 G, magnetic stresses terminate the Keplerian flow close to the stellar surface. Here we report the results of detailed numerical modeling of the magnetic field structure near such neutron stars, taking into account the electrical currents flowing in the disk and magnetosphere as well as in the star and the twisting of the magnetic field caused by the motion of the disk plasma relative to the neutron star.
|Original language||English (US)|
|Number of pages||6|
|Journal||Astrophysical Letters and Communications|
|State||Published - Dec 1 1996|
ASJC Scopus subject areas
- Astronomy and Astrophysics