  A new type of wind - a conical wind - has been discovered in axisymmetric
magnetohydrodynamic simulations of the disk-magnetosphere interaction in cases
where the magnetic field of the star is bunched into an X-type configuration.
Such a configuration arises if the effective viscosity of the disk is larger
than the effective diffusivity, or if the accretion rate in the disk is
enhanced. Conical outflows flow from the inner edge of the disk into a narrow
shell with half-opening angle of 30-45 degrees. The outflow carries about
0.1-0.3 of the disk mass accretion rate and part of the disk's angular
momentum. The conical winds are driven by the gradient of the magnetic pressure
which exists above the disk due to the winding of the stellar magnetic field.
Exploratory 3D simulations show that conical winds are symmetric about rotation
axis of the disk even if the magnetic dipole is significantly misaligned with
the disk's rotation axis. Conical winds appear around stars of different
periods. However, in the case of a star in the "propeller" regime, an
additional - much faster component appears: an axial jet, where matter is
accelerated up to very high velocities at small distances from the star by
magnetic pressure force above the surface of the star. The simulations are done
in dimensionless units and are applicable to a variety of the disk-accreting
magnetized stars: young stars, white dwarfs, neutron stars, and possibly black
holes. For the case of young stars, conical winds and axial jets may appear in
different cases, including Class I young stars, classical T Tauri stars, and
EXors. In EXors periods of enhanced accretion may lead to the formation of
conical winds which correspond to the outflows observed from these stars.
