Evolution of Global Magnetic Fields in Main Sequence A and B Stars

Details Evolution of Global Magnetic Fields in Main Sequence A and B Stars Evolution of Global Magnetic Fields in Main Sequence A and B Stars

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..405..505l&link_type=abstract

Solar Polarization 5: In Honor of Jan Stenflo ASP Conference Series, Vol. 405, proceedings of the conference held 17-21 Septembe

Astronomy and Astrophysics

Astronomy

Scientific paper

Some main sequence A and B stars (``magnetic Ap stars") possess kG-strength global fields of simple geometry. These fields are expected to evolve during the main sequence lifetime of the stars due to ohmic decay, large-scale circulation flows, and the changing stellar structure caused by stellar evolution. We are attempting to obtain useful observational constraints on field evolution by observing the fields of a large sample of magnetic Ap stars in open clusters, from which we derive stellar ages. Our data to date indicate that the fields of these stars decline with stellar age more rapidly than would be expected from magnetic flux conservation as the stars expand with evolution.

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