期刊
ASTRONOMY & ASTROPHYSICS
卷 636, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201937398
关键词
asteroseismology; waves; stars: magnetic field; stars: oscillations; stars: rotation
资金
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program [647383, 670519]
- CNES PLATO grant at CEA/DAp
Context. Stellar internal magnetic fields have recently been shown to leave a detectable signature on period spacing patterns of gravity modes.Aims. We aim to investigate the effect of the obliquity of a mixed (poloidal and toroidal) dipolar internal fossil magnetic field with respect to the rotation axis on the frequency of gravity modes in rapidly rotating stars.Methods. We used the traditional approximation of rotation to compute non-magnetic modes, and a perturbative treatment of the magnetic field to compute the corresponding frequency shifts. We applied the new formalism to HD 43317, a magnetic, rapidly rotating, slowly pulsating B-type star, whose field has an obliquity angle of about 80 degrees .Results. We find that frequency shifts induced by the magnetic field on high-radial-order gravity modes are larger with increasing obliquity angle, when the magnetic axis is closer to the equatorial region, where these modes are trapped. The maximum value is reached for an obliquity angle of 90 degrees. This trend is observed for all mode geometries.Conclusions. Our results predict that the signature of an internal oblique dipolar magnetic field is detectable using asteroseismology of gravity modes.
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