  During the lifetime of sun-like or low mass stars a significant amount of
angular momentum is removed through magnetised stellar winds. This process is
often assumed to be governed by the dipolar component of the magnetic field.
However, observed magnetic fields can host strong quadrupolar and/or octupolar
components, which may influence the resulting spin-down torque on the star. In
Paper I, we used the MHD code PLUTO to compute steady state solutions for
stellar winds containing a mixture of dipole and quadrupole geometries. We
showed the combined winds to be more complex than a simple sum of winds with
these individual components. This work follows the same method as Paper I,
including the octupole geometry which increases the field complexity but also,
more fundamentally, looks for the first time at combining the same symmetry
family of fields, with the field polarity of the dipole and octupole geometries
reversing over the equator (unlike the symmetric quadrupole). We show, as in
Paper I, that the lowest order component typically dominates the spin down
torque. Specifically, the dipole component is the most significant in governing
the spin down torque for mixed geometries and under most conditions for real
stars. We present a general torque formulation that includes the effects of
complex, mixed fields, which predicts the torque for all the simulations to
within 20% precision, and the majority to within ~5%. This can be used as an
input for rotational evolution calculations in cases where the individual
magnetic components are known.
