C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:18:10

2013A&A...550A..84K - Astronomy and Astrophysics, volume 550A, 84-84 (2013/2-1)

Magnetic field topology of the RS CVn star II Pegasi.


Abstract (from CDS):

The dynamo processes in cool active stars generate complex magnetic fields responsible for prominent surface stellar activity and variability at different time scales. For a small number of cool stars magnetic field topologies were reconstructed from the time series of spectropolarimetric observations using the Zeeman Doppler imaging (ZDI) method, often yielding surprising and controversial results. In this study we follow a long-term evolution of the magnetic field topology of the RS CVn binary star IIPeg using a more self-consistent and physically more meaningful modelling approach compared to previous ZDI studies. We collected high-resolution circular polarisation observations of IIPeg using the SOFIN spectropolarimeter at the Nordic Optical Telescope. These data cover 12 epochs spread over 7 years, comprising one of the most comprehensive spectropolarimetric data sets acquired for a cool active star. A multi-line diagnostic technique in combination with a new ZDI code is applied to interpret these observations. We have succeeded in detecting clear magnetic field signatures in average Stokes V profiles for all 12 data sets. These profiles typically have complex shapes and amplitudes of ∼10–3 of the unpolarised continuum, corresponding to mean longitudinal fields of 50-100G. Magnetic inversions using these data reveals evolving magnetic fields with typical local strengths of 0.5-1.0kG and complex topologies. Despite using a self-consistent magnetic and temperature mapping technique, we do not find a clear correlation between magnetic and temperature features in the ZDI maps. Neither do we confirm the presence of persistent azimuthal field rings found in other RSCVn stars. Reconstruction of the magnetic field topology of IIPeg reveals significant evolution of both the surface magnetic field structure and the extended magnetospheric field geometry on the time scale covered by our observations. From 2004 to 2010 the total field energy drastically declined and the field became less axisymmetric. This also coincided with the transition from predominantly poloidal to mainly toroidal field topology. A qualitative comparison of the ZDI maps of IIPeg with the prediction of dynamo theory suggests that the magnetic field in this star is produced mainly by the turbulent α2 dynamo rather than the solar αΩ dynamo. Our results do not show a clear active longitude system, nor is there evidence of the presence of an azimuthal dynamo wave.

Abstract Copyright:

Journal keyword(s): polarization - stars: activity - stars: atmospheres - stars: magnetic field - stars: individual: II Pegasi

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 HD 22468 RS* 03 36 47.2911034958 +00 35 15.938962144 7.09 6.63   5.4   K2:Vnk 1124 0
2 HD 36705 TT* 05 28 44.8916324761 -65 26 55.289846904 8.259 7.856 6.999 6.496 5.993 K0V 931 0
3 V* LQ Hya BY* 09 32 25.5684079124 -11 11 04.687410738 9.316 8.761 7.891 7.288 6.815 K1Vp 401 0
4 V* RS CVn Al* 13 10 36.9078781154 +35 56 05.587686902 8.57 8.51 7.93 7.7   F6IV+G8IV 684 0
5 * gam Equ a2* 21 10 20.5001160337 +10 07 53.682085548 5.03 4.94 4.68 4.43 4.32 A9VpSrCrEu 513 0
6 HD 224085 RS* 23 55 04.0516465022 +28 38 01.248194500 8.88 8.20   6.9   K2+IVeFe-1 679 0

    Equat.    Gal    SGal    Ecl

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