August 7-10, 2017


Magnetic Stars Observed by BRITE

Matthew Shultz (Uppsala University)

G. A. Wade, Royal Military College C. Neiner, LESIA, Observatoire de Paris O. Kochukhov, Uppsala University

Stellar magnetism takes different forms across the HRD, from the highly dynamic dynamo-generated fields that are essentially ubiquitious amongst cool stars, to the rare, stable fossil fields of hot stars. In this talk I will provide an overview of the general properties of magnetic stars, with a focus on the magnetic hot stars that have been observed by BRITE and the BRITEpol spectropolarimetric survey. Magnetic fields provide a number of unique physical constraints, in particular rotational periods, which are often difficult to determine for non-magnetic stars. The diverse phenomena caused or influenced by stellar magnetism additionally make magnetic stars important laboratories for stellar astrophysics. Many magnetic stars exhibit photometric variations associated with their magnetic fields, due to chemical abundance spots or magnetospheric eclipses, which provide a window into radiative diffusion and the physics of magnetospheric plasma transport. Many of the hot, magnetic stars are pulsators, opening the possibility of placing powerful constraints on stellar structure via combining asteroseismological and magnetic analyses. Other early-type magnetic stars are in binary systems, and so offer the opportunity to explore the interplay of tidal interactions and magnetic braking with orbital, rotational, and stellar evolution; and to examine the consequences of magnetic fields for stellar structure by comparing stars with similar stellar parameters and evolutionary statuses, differing only in that one of the stars is magnetic.

Mode of presentation need to be confirmed by the SOC