Reference : New magnetic field measurements of beta Cephei stars and slowly pulsating B stars
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/31745
New magnetic field measurements of beta Cephei stars and slowly pulsating B stars
English
Hubrig, S. [European Southern Observatory, Casilla 19001, Santiago 19, Chile; Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany]
Briquet, Maryline mailto [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium]
De Cat, P. [Koninklijke Sterrenwacht van Belgium, Ringlaan 3, B-1180 Brussel, Belgium]
Schöller, M. [European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany]
Morel, Thierry mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Ilyin, I. [Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany]
1-Apr-2009
Astronomische Nachrichten
Wiley
330
317
Yes (verified by ORBi)
International
0004-6337
1521-3994
Berlin
Germany
[en] stars: early types ; stars: fundamental parameters ; stars: individual (δ Cet ; \xi1 CMa ; 15 CMa ; V1449 Aql ; 53 Psc ; CG Hyi ; 33 Eri ; 40 Tau ; V1143 Tau ; V1144 Tau ; γ Col ; HY Vel ; V335 Vel ; V847 Ara ; V1070Ṡco ; V1092 Sco ; α 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 β 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 β Cephei stars and two stars suspected to be β 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 β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β 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)).
http://hdl.handle.net/2268/31745
also: http://hdl.handle.net/2268/117882
10.1002/asna.200811187
http://adsabs.harvard.edu/abs/2009AN....330..317H
http://de.arxiv.org/abs/0902.1314

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