First magnetic field models for recently discovered magnetic $beta$,Cephei and slowly pulsating B stars

S. Hubrig$^1$, I. Ilyin$^1$, M. Sch"oller$^2, M. Briquet$^3, T. Morel$^4, P. De Cat$^5$

$^1$ Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
$^2$ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei M"unchen, Germany
$^3$ Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001~Leuven, Belgium
$^4$ Institut d'Astrophysique et de G'eophysique, Universit'e de Li`ege, All'ee du 6 Ao^ut, B^at. B5c, 4000~Li`ege, Belgium
$^5$ Koninklijke Sterrenwacht van Belgi"e, Ringlaan 3, 1180 Brussel, Belgium

In spite of recent detections of magnetic fields in a number of $beta$,Cephei
and slowly pulsating B (SPB) stars, their impact on stellar rotation, pulsations,
and element diffusion is not sufficiently studied yet.
The reason for this is the lack of knowledge of rotation periods, the magnetic
field strength distribution and temporal variability, and the field geometry.
New longitudinal field measurements of four $beta$,Cephei and
candidate $beta$,Cephei stars, and two SPB stars were acquired with FORS,2 at the VLT.
These measurements allowed us to carry out a search for rotation periods and to
constrain the magnetic field geometry for four stars in our sample.

Reference: ApJ 726, L5
Status: Manuscript has been accepted