Volume 591, July 2016
|Number of page(s)||15|
|Section||Stellar structure and evolution|
|Published online||13 June 2016|
The different origins of magnetic fields and activity in the Hertzsprung gap stars, OU Andromedae and 31 Comae⋆
1 Institute of Astronomy, Bulgarian Academy of Sciences, 71 Tsarigradsko Shosse blvd, 1784 Sofia, Bulgaria
2 Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, 31400 Toulouse, France
3 CNRS, UMR 5277, Institut de Recherche en Astrophysique et Planétologie, 14 Av. Édouard Belin, 31400 Toulouse, France
4 Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
5 Saint Petersburg State University, Saint Petersburg, Universitetski pr. 28, 198504 Saint Petersburg, Russia
6 Observatório Nacional/MCTI, Rua General José Cristino 77, 20921-400 Rio de Janeiro, Brazil
Received: 12 June 2015
Accepted: 20 March 2016
Context. When crossing the Hertzsprung gap, intermediate-mass stars develop a convective envelope. Fast rotators on the main sequence, or Ap star descendants, are expected to become magnetic active subgiants during this evolutionary phase.
Aims. We compare the surface magnetic fields and activity indicators of two active, fast rotating red giants with similar masses and spectral class but different rotation rates – OU And (Prot = 24.2 d) and 31 Com (Prot = 6.8 d) – to address the question of the origin of their magnetism and high activity.
Methods. Observations were carried out with the Narval spectropolarimeter in 2008 and 2013. We used the least-squares deconvolution (LSD) technique to extract Stokes V and I profiles with high signal-to-noise ratio to detect Zeeman signatures of the magnetic field of the stars. We then provide Zeeman-Doppler imaging (ZDI), activity indicators monitoring, and a precise estimation of stellar parameters. We use state-of-the-art stellar evolutionary models, including rotation, to infer the evolutionary status of our giants, as well as their initial rotation velocity on the main sequence, and we interpret our observational results in the light of the theoretical Rossby numbers.
Results. The detected magnetic field of OU Andromedae (OU And) is a strong one. Its longitudinal component Bl reaches 40 G and presents an about sinusoidal variation with reversal of the polarity. The magnetic topology of OU And is dominated by large-scale elements and is mainly poloidal with an important dipole component, as well as a significant toroidal component. The detected magnetic field of 31 Comae (31 Com) is weaker, with a magnetic map showing a more complex field geometry, and poloidal and toroidal components of equal contributions. The evolutionary models show that the progenitors of OU And and 31 Com must have been rotating at velocities that correspond to 30 and 53%, respectively, of their critical rotation velocity on the zero age main sequence. Both OU And and 31 Com have very similar masses (2.7 and 2.85 M⊙, respectively), and they both lie in the Hertzsprung gap.
Conclusions. OU And appears to be the probable descendant of a magnetic Ap star, and 31 Com the descendant of a relatively fast rotator on the main sequence. Because of the relatively fast rotation in the Hertzsprung gap and the onset of the development of a convective envelope, OU And also has a dynamo in operation.
Key words: stars: individual: OU Andromedae / stars: individual: 31 Comae / stars: late-type / stars: magnetic field
© ESO, 2016
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