Abstract

It has been known for many years that stars possess surface magnetic fields of considerable strength. Up to the present, not only detailed characteristics of individual magnetic stars but also their statistical properties have been revealed by observations. From a theoretical point of view, the importance of the magnetic effects on stellar evolution has also long been noticed. In particular, magnetic stress is regarded as the prime possibility for internal angular momentum transport. Despite the significance, however, theoretical understanding of the evolution of the magnetic stars has been limited. This is due to the difficulty of treating stellar magnetic fields in a physically consistent manner, and it is the reason why we have been working on modeling magneto-rotational stellar evolution. Recently, we have proposed a new framework for stellar evolution simulations in which the interplay between magnetic field, rotation, mass loss, and changes in the stellar density and temperature distributions are treated self-consistently. In this talk, I will present the essence of the modeling and show the results of the first application to the 1.5 Msun magneto-rotational evolution.