Open AccessSurface differential rotation and photospheric magnetic field of the young solar‐type star HD 171488 (V889 Her)
Author(s) -
Marsden S. C.,
Donati J.F.,
Semel M.,
Petit P.,
Carter B. D.
Publication year - 2006
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.1365-2966.2006.10503.x
Subject(s) - physics , differential rotation , astrophysics , polar , brightness , zeeman effect , azimuth , starspot , magnetic field , astronomy , stars , quantum mechanics
ABSTRACT We present spectropolarimetric observations of the young, single early G‐dwarf HD 171488. These observations were obtained over a five‐night period in 2004 September at the 3.9‐m Anglo‐Australian Telescope using the SEMPOL spectropolarimeter visitor instrument. Using the technique of least‐squares deconvolution to increase the signal‐to‐noise ratio of the data, we have applied Zeeman Doppler imaging to reconstruct brightness and magnetic surface topologies of the star. The brightness image shows a large polar spot with weaker low‐ to mid‐latitude features, confirming an earlier Doppler imaging observation. The reconstruction of the surface magnetic field shows regions of radial field at all latitudes (except near the pole) and regions of azimuthal field predominantly at high latitudes (60°–70°), with the azimuthal field almost forming a ring around the polar regions. We have incorporated a solar‐like differential rotation law into the imaging process to determine the surface differential rotation of cool spots on HD 171488. This gives an equatorial rotation rate of 1.313 ± 0.004 d and a surface shear of dΩ= 0.402 ± 0.044 rad d −1 . This means that the equator of HD 171488 laps the poles every ∼16 ± 2 d and that HD 171488 has a photospheric shear approximately seven times the solar value. This is the largest measurement of surface differential rotation yet obtained using the Doppler imaging method and is over twice the value of previously observed early G‐dwarfs.