| Abstract | We report the detection of a strong, reversing magnetic field and variable Ha emission in the bright helium-weak star HD 176582 (HR 7185). Spectrum, magnetic, and photometric variability of the star are all consistent with a precisely determined period of 1.5819840 +/- 0.0000030 days which we assume to be the rotation period of the star. From the magnetic field curve, and assuming a simple dipolar field geometry, we derive a polar field strength of approximately 7 kG and a lower limit of 52 degrees for the inclination of the rotation axis. However, based on the behavior of the Ha emission, we adopt a large inclination angle of 85 degrees and this leads to a large magnetic obliquity of 77 degrees. The Ha emission arises from two distinct regions located at the intersections of the magnetic and rotation equators and which corotate with the star at a distance of about 3.5 R(*) above its surface. We estimate that the emitting regions have radial and meridional sizes on the order of 2 R(*) and azimuthal extents ( perpendicular to the magnetic equator) of less than approximately 0.6 R(*). HD 176582 therefore appears to show many of the cool magnetospheric phenomena as that displayed by other magnetic helium-weak and helium-strong stars such as the prototypical helium-strong star sigma Ori E. The observations are consistent with current models of magnetically confined winds and rigidly rotating magnetospheres for magnetic Bp stars. |
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