... material

Note also that a fraction of the open poloidal flux initially tied to the primary's progenitor could remain trapped by the accretion flow.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... comparable

Full computations of MAES show that the three magnetic field components are comparable at the disc surface, namely $B_\phi^+ \sim B_r^+ \sim B_z$ (Ferreira & Pelletier 1995; Ferreira 1997).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... SAD

It has been recently showed that a previously claimed instability of accretion-ejection structures does not apply to this type of solution (see Königl 2004, and references therein).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.