[en] stars: early types ; stars: fundamental parameters ; stars: individual (Î´ Cet ; \xi1 CMa ; 15 CMa ; V1449 Aql ; 53 Psc ; CG Hyi ; 33 Eri ; 40 Tau ; V1143 Tau ; V1144 Tau ; Î³ Col ; HY Vel ; V335 Vel ; V847 Ara ; V1070á¹ co ; V1092 Sco ; Î± Tel ; V338 Sge ; V4199 Sgr ; V4372 Sgr ; DK Oct ; 21 CMa ; HR 6320) ; stars: magnetic fields ; stars: oscillations
[en] We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B-type stars consisting of confirmed or candidate Î² Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B-type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three Î² Cephei stars and two stars suspected to be Î² Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3Ï has been diagnosed in two normal B-type stars, the nitrogen-rich early B-type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of Î² Cephei stars have detected magnetic fields: Out of 13 Î² Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected Î² Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non-magnetic pulsating stars in the H-R diagram. We find that their domains in the H-R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i-values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars. Based on observations obtained at the European Southern Observatory, Paranal, Chile (ESO programmes 078.D-0140(A), 078.D-0330(A), 079.D-0241(A), and 080.D-0383(A)).