EDP Sciences
Free Access
Volume 444, Number 2, December III 2005
Page(s) L29 - L32
Section Letters
DOI https://doi.org/10.1051/0004-6361:200500203
Published online 25 November 2005

A&A 444, L29-L32 (2005)
DOI: 10.1051/0004-6361:200500203


Probing the internal magnetic field of slowly pulsating B-stars through g modes

S. S. Hasan1, J.-P. Zahn2 and J. Christensen-Dalsgaard3

1  Indian Institute of Astrophysics, Koramangala, Bangalore-560034, India
    e-mail: hasan@iiap.res.in
2  LUTH, Observatoire de Paris, 92195 Meudon, France
3  Institut for Fysik og Astronomi, Aarhus Universitet, 8000 Aarhus C, Denmark

(Received 28 July 2005 / Accepted 22 October 2005 )

Aims.We suggest that high-order g modes can be used as a probe of the internal magnetic field of SPB (slowly pulsating B) stars. The idea is based on earlier work by the authors hich analytically investigated the effect of a vertical magnetic field on p and g modes in a plane-parallel isothermal stratified atmosphere. It was found that even a weak field can significantly shift the g-mode frequencies - the effect increases with mode order.
Methods.In the present study we adopt the classical perturbative approach to estimate the internal field of a 4 solar mass SPB star by looking at its effect on a low-degree (l=1) and high-order (n=20) g mode with a period of about 1.5 d.
Results.We find that a polar field strength of about 110 kG on the edge of the convective core is required to produce a frequency shift of 1%. Frequency splittings of that order have been observed in several SPB variables, in some cases clearly too small to be ascribed to rotation. We suggest that they may be due to a poloidal field with a strength of order 100 kG, buried in the deep interior of the star.

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© ESO 2005

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