Chapters 4 and 5 discussed various aspects of the interaction between the magnetic field and the thermal-gravitational-rotational fields in different stellar domains. This chapter broadens the discussion with an eye to the understanding of those early-type stars, numbering over 200, which show surface magnetic fields, detectable through the Zeeman effect. The discussion covers the stability of large-scale stellar magnetic fields; the dynamics of the oblique rotator and the Eulerian nutation and the consequent internal motions; non-uniform rotation and the oblique rotator model; models of...

Chapters 4 and 5 discussed various aspects of the interaction between the magnetic field and the thermal-gravitational-rotational fields in different stellar domains. This chapter broadens the discussion with an eye to the understanding of those early-type stars, numbering over 200, which show surface magnetic fields, detectable through the Zeeman effect. The discussion covers the stability of large-scale stellar magnetic fields; the dynamics of the oblique rotator and the Eulerian nutation and the consequent internal motions; non-uniform rotation and the oblique rotator model; models of rotating magnetic stars; magnetic torques acting on the oblique rotator and spin-down, spin-up, and changes in obliquity; the origin of the field; abundance anomalies; and the rapidly oscillating Ap (roAp) phenomenon.