We present a non-axisymmetric oblique rotator model for the magnetic field geometry of the star HD 154708 which at the same time fits the magnetic variations — longitudinal magnetic field and field modulus — and the intensity profiles of selected Si I lines in the infrared. It turns out that only by discarding the usual assumption of an axisymmetric magnetic field configuration can field ratios, phase shifts and line profiles be corre

Modelling the Magnetic Field Geometry of the Rapidly Oscillating Star HD 154708 with an Extraordinarily Strong Magnetic Field

LEONE, Francesco;
2013-01-01

Abstract

We present a non-axisymmetric oblique rotator model for the magnetic field geometry of the star HD 154708 which at the same time fits the magnetic variations — longitudinal magnetic field and field modulus — and the intensity profiles of selected Si I lines in the infrared. It turns out that only by discarding the usual assumption of an axisymmetric magnetic field configuration can field ratios, phase shifts and line profiles be corre
2013
978-1-58381-842-8
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11769/84951
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