Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-12-07
Mon.Not.Roy.Astron.Soc. 354 (2004) 591-600
Astronomy and Astrophysics
Astrophysics
11 pages, 10 figures
Scientific paper
10.1111/j.1365-2966.2004.08219.x
We present a time-dependent model of the interaction between a neutron star magnetosphere and a thin (Shakura-Sunyaev) accretion disc, where the extent of the magnetosphere is determined by balancing outward diffusion and inward advection of the stellar magnetic field at the inner edge of the disc. The nature of the equilibria available to the system is governed by the magnetic Prandtl number Pm and the ratio \xi of the corotation radius to the Alfven radius. For \xi > Pm^0.3, the system can occupy one of two stable states, where the torques are of opposite signs. If the star is spinning up initially, in the absence of extraneous perturbations, \xi decreases until the spin-up equilibrium vanishes, the star subsequently spins down, and the torque asymptotes to zero. Vortex-in-cell simulations of the Kelvin-Helmholtz instability suggest that the transport speed across the mixing layer between the disc and magnetosphere is less than the shear speed when the layer is thin, unlike in previous models.
Locsei Janos Tobias
Melatos Andrew
No associations
LandOfFree
Torque bistability in the interaction between a neutron star magnetosphere and a thin accretion disc does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Torque bistability in the interaction between a neutron star magnetosphere and a thin accretion disc, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Torque bistability in the interaction between a neutron star magnetosphere and a thin accretion disc will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-76354