  We consider the general problem of a Parker-type non-relativistic isothermal
wind from a rotating and magnetic star. Using the magnetohydrodynamics (MHD)
code athena++, we construct an array of simulations in the stellar rotation
rate $\Omega_\ast$ and the isothermal sound speed $c_T$, and calculate the
mass, angular momentum, and energy loss rates across this parameter space. We
also briefly consider the three dimensional case, with misaligned magnetic and
rotation axes.
  We discuss applications of our results to the spindown of normal stars,
highly-irradiated exoplanets, and to nascent highly-magnetic and
rapidly-rotating neutron stars born in massive star core collapse.8
