Magnetic Fields in Massive Stars, Their Winds, and Their Nebulae

摘要: Massive stars are crucial building blocks of galaxies and the universe, as production sites heavy elements stirring agents energy providers through stellar winds supernovae. The field magnetic massive has seen tremendous progress in recent years. Different perspectives—ranging from direct measurements over dynamo theory evolution to colliding environment—fruitfully combine into a most interesting still evolving overall picture, which we attempt review here. Zeeman signatures leave no doubt that at least some O- early B-type have surface field. Indirect evidence, especially non-thermal radio emission winds, suggests many more. emerging picture for shows similarities with results intermediate mass stars, much more data available. Observations often compatible dipole or low order multi-pole about 1 kG (O-stars) 300 G 30 (Ap/Bp stars). Weak unordered fields been detected O-star ζ Ori A Vega, first normal A-type star Theory offers essentially two explanations origin observed fields: fossil fields, particularly strong ordered different mechanisms, preferentially less fields. Numerical simulations yield concrete stable (fossil) configuration, but give contradictory whether action radiative envelope main sequence is possible. Internal may not even show up surface, affect they lead uniform rotation, slowly rotating cores faster rotation. Surface metallicities become enhanced, thus affecting mass-loss rates.