Open AccessMagnetic topology and surface differential rotation on the K1 subgiant of the RS CVn system HR 1099
Author(s) -
Petit P.,
Donati J.F.,
Wade G. A.,
Landstreet J. D.,
Bagnulo S.,
Lüftinger T.,
Sigut T. A. A.,
Shorlin S. L. S.,
Strasser S.,
Aurière M.,
Oliveira J. M.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07420.x
Subject(s) - physics , differential rotation , subgiant , dynamo , starspot , stellar rotation , astrophysics , brightness , rotation (mathematics) , magnetic field , dynamo theory , late type star , stars , astronomy , stellar atmosphere , geometry , mathematics , globular cluster , quantum mechanics
We present here spectropolarimetric observations of the RS CVn system HR 1099 (V711 Tau) secured from 1998 February to 2002 January with the spectropolarimeter MuSiCoS at the Télescope Bernard Lyot (Observatoire du Pic du Midi, France). We apply Zeeman–Doppler imaging and reconstruct surface brightness and magnetic topologies of the K1 primary subgiant of the system, at five different epochs. We confirm the presence of large, axisymmetric regions where the magnetic field is mainly azimuthal, providing further support to the hypothesis that dynamo processes may be distributed throughout the whole convective zone in this star. We study the short‐term evolution of surface structures from a comparison of our images with observations secured at close‐by epochs by Donati et al. at the Anglo‐Australian Telescope. We conclude that the small‐scale brightness and magnetic patterns undergo major changes within a time‐scale of 4–6 weeks, while the largest structures remain stable over several years. We report the detection of a weak surface differential rotation (both from brightness and magnetic tracers) indicating that the equator rotates faster than the pole with a difference in rotation rate between the pole and the equator about four times smaller than that of the Sun. This result suggests that tidal forces also affect the global dynamic equilibrium of convective zones in cool active stars.