The propeller regime of disk accretion to a rapidly rotating magnetized star


PROPELLER-DRIVEN OUTFLOWS AND DISK OSCILLATIONS Authors: M.M. Romanova, G.V. Ustyugova, A.V. Koldoba, R.V.E. Lovelace. [return]

Example of matter flow in the ``high" state (at t/P₀=924). The color background shows the density distribution which changes from red r=1.5 to blue r=0.0005. The solid black lines are magnetic field lines. The dark-blue lines/arrows are streamlines of the matter flow with the length of arrows proportional to velocity. The bold red line shows the surface where the matter pressure equals to magnetic pressure. Parameters: m=10, W=1, a_vis=0.3, a_dif=0.2.

Color background and streamlines show fluxes of angular momentum carried by the matter (left panel) and by the field (right panel) in the "high" state t/P₀=924. Note that the scales are different, because N_f is very large near the surface of the star. However, the total integrated fluxes N_m and N_f have comparable values. Parameters: m=10, W=1, a_vis=0.3, a_dif=0.2.

Left panel: Fluxes to/out of the star: matter flux (red), angular momentum flux associated with matter (green), angular momentum flux associated with magnetic field (blue). Right panel: Fluxes to the wind/jet: matter flux (red), angular momentum flux associated with matter (green), angular momentum flux associated with magnetic field (blue). Parameters: m=10, W=1, a_vis=0.3, a_dif=0.2.

The case of larger viscosity (a_vis=0.6, a_dif=0.2) when oscillations are well-tuned.
Left panel: Variation of matter flux to the star (red) and to the jet/wind (blue) with time.
Right panel: Variation of the angular momentum flux from the star (red) and to the jet/wind (blue) with time.

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