Radiative transfer dynamo effect
  Magnetic fields in rotating and radiating astrophysical plasma can be
produced due to a radiative interaction between plasma layers moving relative
to each other. The efficiency of current drive, and with it the associated
dynamo effect, is considered in a number of limits. It is shown here, however,
that predictions for these generated magnetic fields can be significantly
higher when kinetic effects, previously neglected, are taken into account.
