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Magnetic Doppler Imaging of He-strong star HD 184927

Published online by Cambridge University Press:  07 August 2014

I. Yakunin
Affiliation:
Special Astrophysical Observatory, Nizhniy Arkhyz, Russia369167
G. Wade
Affiliation:
Department of Physics, Royal Military College of Canada, P.O. Box 17000, Station Forces, Kingston, Ontario, Canada, K7K 7B4
D. Bohlender
Affiliation:
National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada
O. Kochukhov
Affiliation:
Department of Physics and Astronomy, Uppsala University, SE-751 20, Uppsala, Sweden
V. Tsymbal
Affiliation:
Tavrian National University, Vernadskiys Avenue 4, Simferopol, Crimea, 95007, Ukraine
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Abstract

We have employed an extensive new timeseries of Stokes I and V spectra obtained with the ESPaDOnS spectropolarimeter at the 3.6-m Canada-France-Hawaii Telescope to investigate the physical parameters, chemical abundance distributions and magnetic field topology of the slowly-rotating He-strong star HD 184927. We infer a rotation period of 9d .53071 ± 0.00120 from Hα, Hβ, LSD magnetic measurements and EWs of helium lines. We used an extensive NLTE TLUSTY grid along with the SYNSPEC code to model the observed spectra and find a new value of luminosity. In this poster we present the derived physical parameters of the star and the results of Magnetic Doppler Imaging analysis of the Stokes I and V profiles. Wide wings of helium lines can be described only under the assumption of the presence of a large, very helium-rich spot.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

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