MHD SIMULATIONS OF DISK  MAGNETIZED STAR INTERACTIONS IN QUIESCENT REGIME: FUNNEL FLOWS AND ANGULAR MOMENTUM TRANSPORT Authors: Romanova, M.M., Ustyugova, G.V., Koldoba, A.V., Lovelace R.V.E. 

Close view of a quasistationary funnel flow calculated for Type I initial conditions. The color background represents the logarithm of the density. The density has a minimum value r = 0.004 (blue) and a maximum value r = 2 (red). The lines are poloidal magnetic field lines or equivalently Y(r; z) = const lines. The arrows represent the poloidal mass flux density rv. The bold dark line is the field line approximately in the middle of the funnel flow. The variation of different quantities along this field line are shown in subsequent figures.

Density and poloidal magnetic field lines for a case with outflows. The magnetic moment of the star m = 5.3 is 5 times larger than that used in most of our simulations. The density in the corona is 3 times smaller than in other simulations. Color background represents the density, white solid lines  contours of magnetic ux, black solid line is the line ~ b = 1. Level lines of density are exponentially distributed between the minimum, r = 4 x 10^{4} and the maximum, r = 17.6 values. The Y lines are exponentially distributed between Y = 0.1 and Y= 3. Arrows are velocities. The grid used was NR x Nq = 110 x 71, and the viscosity parameter was a = 0.01.
