FIRST MAGNETIC FIELD MODELS FOR RECENTLY DISCOVERED MAGNETIC {beta} CEPHEI AND SLOWLY PULSATING B STARS

Journal Article · Sat Jan 01 04:00:00 EST 2011 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/726/1/L5· OSTI ID:21560592

Hubrig, S; Ilyin, I ^[1]; Schoeller, M ^[2]; Briquet, M ^[3]; Morel, T ^[4]

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1. Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam (Germany)
2. European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei Muenchen (Germany)
3. Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven (Belgium)
4. Institut d'Astrophysique et de Geophysique, Universite de Liege, Allee du 6 Aout, Bat. B5c, 4000 Liege (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 has not yet been sufficiently studied. 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 Very Large Telescope. 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.

• OSTI ID: 21560592
• Journal Information: Astrophysical Journal Letters, Journal Name: Astrophysical Journal Letters Journal Issue: 1 Vol. 726; ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
DIFFUSION
MAGNETIC FIELDS
MOTION
PULSATIONS
ROTATION
STARS