  Magnetic field generation in the Sun and solar-type stars is modeled here
based on the formation of magnetically polarized condensates (B. M. Mirza, Mod.
Phys. Lett. B 28 (2014) 1450148) under the high density and pressure
conditions. The correct orders of magnitude for the time period and the energy
loss in a solar cycle are deduced, as well as the enhancement in the energy
emission observed during solar cycles. It is shown that this feedback magnetic
field along with differential rotation is sufficient to generate the toroidal
magnetic field in the solar exterior. The model is useful in determining
magnetic polarity reversals, energy generation, and reversal times, in
solar-type stars.
