Observations of non-solar-type dynamo processes in stars with shallow convective zones

Details Observations of non-solar-type dynamo processes in stars with shallow convective zones Observations of non-solar-type dynamo processes in stars with shallow convective zones

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.411.1301j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 411, Issue 2, pp. 1301-1312.

Astronomy and Astrophysics

Astronomy

9

Stars: Activity, Stars: Individual: Hd 171488, Stars: Magnetic Field, Stars: Solar-Type, Starspots

Scientific paper

The magnetic field topology and differential rotation are fundamental signatures of the dynamo processes that generate the magnetic activity observed in the Sun and solar-type stars. To investigate how these dynamo processes evolve in stars with shallow convective zones, we present high-resolution spectropolarimetric observations of the young GO dwarf HD 171488 over three epochs. Using the Zeeman-Doppler tomographic imaging technique, we have reconstructed surface brightness images that are dominated by polar and high-latitude starspots and a magnetic field topology that shows large-scale radial and azimuthal magnetic field components. Over the time-span of our observations, we do not observe a reversal of the magnetic field polarity as has been observed in other solar-type stars with shallow convective zones. The phase coverage of our data was sufficient to determine the differential rotation for two epochs where in conjunction with previous work, we conclude that there is no evidence for the temporal evolution of differential rotation. Spectropolarimetric observations were obtained, from 2007 May 21-26, 2007 November 8-13 and 2008 May 26-30 with the NARVAL echelle spectropolarimeter at the Telescope Bernard Lyot (Observatoire du Pic du Midi, France).

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