Modeling of magneto-rotational stellar evolution

While magnetic fields have long been considered to be important for the evolution of non-degenerate stars and compact stars, it has become clear in recent years that actually all are deeply affected. This is particularly true regarding their internal angular momentum distribution, but may also influence mixing processes even fate star. We propose a new framework stellar simulations, which interplay between field, rotation, mass loss, changes density temperature distributions treated self-consistently. For average large-scale symmetric axis rotation star, we derive 1D equations toroidal poloidal components from mean-field MHD equation by applying Alfven's theorem, conservative form transfer due Lorentz force formulated. implement our formalism into numerical code simulate magneto-rotational 1.5 M$_\odot$ stars. The aided $\Omega$ effect imposes torsional Alfven waves propagating through magnetized medium, leading near-rigid within timescale. Our models with different initial spins B-fields can reproduce main observed properties Ap/Bp Calculations continued red-giant regime show pronounced core-envelope coupling, reproduces core surface periods determined asteroseismic observations.