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"PROPELLER" REGIME OF DISK ACCRETION TO RAPIDLY ROTATING STARS Authors: M.M. Romanova, G.V. Ustyugova, A.V. Koldoba, R.V.E. Lovelace. [return] |
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Geometry of disk accretion to a rapidly rotating star with an aligned dipole magnetic field. Top panel shows radial distribution of angular velocities of the star and of the disk. Bottom panel shows schematic structure of the magnetosphere in the propeller regime. |
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| The top panels show the angular momentum flux carried by the field (a) and by the matter (b). The bottom panels show the energy fluxes carried by the field (c) and by the matter (d). The right-hand panels show the angular momentum fluxes close to the star carried by the field (e), by the matter (f), and by the viscous stress (g). The background color indicates the value of the flux while the streamlines indicate the direction of the flux. | |
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In panel (a) the background shows the matter flux and the
lines are the streamlines of the matter flow. The white line is the v = vesc
line. In panel (b) the background shows the plasma parameter β = 8πp/B2.
The streamlines are the magnetic field lines, and the white dashed line shows
the β = 1 line. In panel (c) the background shows r sin θBf,
which for steady conditions is the total poloidal current through a disk ≤ r sin
θ center on the z−axis. The lines are the magnetic field lines. The white dashed
line shows the neutral line where Bp = 0. The bottom panels (d - f) show the
same as (a - c) but in the vicinity of the star. [return]
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