August 7-10, 2017


o Lup: a strongly magnetic B-type star with stellar pulsations

Bram Buysschaert (LESIA - Paris Observatory)

B. Buysschaert (1,2), C. Neiner (1), A.J. Martin (1), M.E. Oksala (1,3), and C. Aerts (2) 1. LESIA, Observatoire de Paris, Meudon, France 2. Institute of Astronomy, KU Leuven, Leuven, Belgium 3. California Lutheran University, Thousand Oaks, CA, USA

About 10% of early-type stars host a detectable and stable large-scale magnetic field at their surface. This field is anticipated to influence the conditions at the surface, the circumstellar environment, and possibly the deep stellar interior. The magnetic fields of early-type stars typically have a simple geometric configuration, often an oblique dipole, with a dipolar strength typically ranging from 100 Gauss up to several kiloGauss. To probe the effect of this field on the deep interior, the star must exhibit a sufficient amount of well characterized stellar pulsations. However, few examples of magnetic pulsators are known, and the occurrence of stellar pulsations in early-type stars does not depend on its magnetic properties. The search for such stars is a part of the BRITE spectropolarimetric survey, which is a complementary study to the constellation of BRITE nano-satellites. The BRITE nano-satellites monitor all stars brighter than V = 4 mag for (periodic) photometric variability, while the BRITE spectropolarimetric survey aims to detect the possible magnetic field for these objects and monitor the rotational modulation induced by them. Here, we report the synergy between both datasets for the B-type star o Lup to characterize its large-scale magnetic field and to interpret its photometric variability.

Mode of presentation need to be confirmed by the SOC