  We discuss magnetic field enhancement by unstable r-modes (driven by the
gravitational radiation reaction force) in rotating stars. In the absence of a
magnetic field, gravitational radiation exponentially increases the r-mode
amplitude $\alpha$, and accelerates differential rotation (secular motion of
fluid elements). For a magnetized star, differential rotation enhances the
magnetic field energy. Rezzolla et al. (2000--2001) argued that if the magnetic
energy grows faster than the gravitational radiation reaction force pumps
energy into the r-modes, then the r-mode instability is suppressed. Chugunov
(2015) demonstrated that without gravitational radiation, differential rotation
can be treated as a degree of freedom decoupled from the r-modes and controlled
by the back reaction of the magnetic field. In particular, the magnetic field
windup does not damp r-modes. Here we discuss the effect of the back reaction
of the magnetic field on differential rotation of unstable r-modes, and show
that it limits the generated magnetic field and the magnetic energy growth rate
preventing suppression of the r-mode instability by magnetic windup at low
saturation amplitudes, $\alpha \ll 1$, predicted by current models.
