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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2011

The strong magnetic field of the large-amplitude beta Cephei pulsator V1449 Aquilae

Résumé


Aims: Only for very few beta Cephei stars has the behaviour of the magnetic field been studied over the rotation cycle. During the past two years we have obtained multi-epoch polarimetric spectra of the beta Cephei star V1449 Aql with SOFIN at the Nordic Optical Telescope to search for a rotation period and to constrain the geometry of the magnetic field.
Methods: The mean longitudinal magnetic field is measured at 13 different epochs. The new measurements, together with the previous FORS 1 measurements, have been used for the frequency analysis and the characterization of the magnetic field.
Results: V1449 Aql so far possesses the strongest longitudinal magnetic field of up to 700 G among the beta Cephei stars. The resulting periodogram displays three dominant peaks with the highest peak at f = 0.0720 d-1 corresponding to a period P = 13ḍ893. The magnetic field geometry can likely be described by a centred dipole with a polar magnetic field strength Bd around 3 kG and an inclination angle beta of the magnetic axis to the rotation axis of 76 ± 4°. As of today, the strongest longitudinal magnetic fields are detected in the beta Cephei stars V1449 Aql and xi1 CMa with large radial velocity amplitudes. Their peak-to-peak amplitudes reach ~90 km s-1 and ~33 km s-1, respectively. Concluding, we briefly discuss the position of the currently known eight magnetic beta Cephei and candidate beta Cephei stars in the Hertzsprung-Russell (H-R) diagram.

Dates et versions

hal-03733057 , version 1 (21-07-2022)

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S. Hubrig, I. Ilyin, Maryline Briquet, Markus Schoeller, Jean-François González, et al.. The strong magnetic field of the large-amplitude beta Cephei pulsator V1449 Aquilae. Astronomy and Astrophysics - A&A, 2011, 531, pp.L20. ⟨10.1051/0004-6361/201117261⟩. ⟨hal-03733057⟩
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