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Title: Discovery of the Magnetic Field of the B1/B2V Star sigma Lupi
Authors: Henrichs, H. F
Kolenberg, Katrien
Plaggenborg, B
Marsden, S. C
Waite, I. A
Landstreet, J
Grunhut, J
Oksala, M
Wade, G
Issue Date: 2012
Publisher: AMER INST PHYSICS
Host Document: STELLAR POLARIMETRY: FROM BIRTH TO DEATH vol:1429 pages:90-93
Conference: Conference on Stellar Polarimetry - From Birth to Death location:Madison: WI date:JUN 27-30, 2011
Abstract: In our search for new magnetic massive stars we use the strongest indirect indicator of a magnetic field in B stars, which is periodic variability of UV stellar wind lines occurring in a velocity range symmetric around zero. Our aim is to obtain follow-up spectropolarimetry to search for a magnetic field in magnetic candidate stars. We quantify UV wind line variability, and analyse its time behaviour. The B1/B2Vstar sigma Lupi emerged as a new magnetic candidate star. AAT spectropolarimetric measurements with SEMPOL were obtained. The stellar wind line variations of sigma Lupi are similar to what is known in magnetic B stars, but no periodicity could be determined. We detected a longitudinal magnetic field with varying strength and amplitude of about 100 G with error bars of typically 20 G, which supports an oblique magnetic-rotator configuration. The equivalent width variations of the UV lines, the magnetic and the optical line variations are consistent with the well-known photometric period of 3.02 days, which we identifywith the rotation period of the star. Additional observations with ESPaDOnS attached to the CFHT strongly confirmed this discovery, and allowed to determine a precise magnetic period. Further analysis revealed that sigma Lupi is a helium-strong star, with an enhanced nitrogen abundance and an underabundance of carbon, and has a spotted surface. We conclude that sigma Lupi is a magnetic oblique rotator, and is a He-strong star. It is the fourth B star for which a magnetic field is discovered from studying only its wind variability. Like in the other magnetic B stars the wind emission originates in the magnetic equator, with maximum emission occurring when a magnetic pole points towards the Earth. The 3.01819 d magnetic rotation period is consistent with the photometric period, with maximum light corresponding to maximum magnetic field. A full paper will be submitted to Astronomy & Astrophysics.
ISSN: 0094-243X
Publication status: published
KU Leuven publication type: IC
Appears in Collections:Institute of Astronomy

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