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Magnetic Field Structure and Activity of the He-burning Giant 37 Comae

Published online by Cambridge University Press:  07 August 2014

S. Tsvetkova ,
P. Petit ,
R. Konstantinova-Antova ,
M. Aurière ,
G. A. Wade ,
C. Charbonnel  and
N. A. Drake
S. Tsvetkova
Affiliation:
Institute of Astronomy and NAO, Bulgarian Academy of Sciences, Bulgaria email: stsvetkova@astro.bas.bg
P. Petit
Affiliation:
IRAP, UMR 5277, CNRS and Université de Toulouse, France
R. Konstantinova-Antova
Affiliation:
Institute of Astronomy and NAO, Bulgarian Academy of Sciences, Bulgaria email: stsvetkova@astro.bas.bg IRAP, UMR 5277, CNRS and Université de Toulouse, France
M. Aurière
Affiliation:
IRAP, UMR 5277, CNRS and Université de Toulouse, France
G. A. Wade
Affiliation:
Department of Physics, Royal Military College of Canada, Ontario, Canada
C. Charbonnel
Affiliation:
IRAP, UMR 5277, CNRS and Université de Toulouse, France Geneva Observatory, University of Geneva, Switzerland
N. A. Drake
Affiliation:
Sobolev Astronomical Institute, St. Petersburg State University, Russia Observatório Nacional/MCTI, Rio de Janeiro, Brazil
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Abstract

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We present the first magnetic map of the late-type giant 37 Com. The Least Squares Deconvolution (LSD) method and Zeeman Doppler Imaging (ZDI) inversion technique were applied. The chromospheric activity indicators Hα, S-index, Ca ii IRT and the radial velocity were also measured. The evolutionary status of the star has been studied on the basis of state-of-the-art stellar evolutionary models and chemical abundance analysis. 37 Com appears to be in the core Helium-burning phase.

Keywords

stars: magnetic fields – stars: abundances – stars: individual: 37 Com

References

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