Volume 523, November-December 2010
|Number of page(s)||12|
|Published online||15 November 2010|
Modelling the molecular Zeeman-effect in M-dwarfs: methods and first results
Institute of Astrophysics, Georg-August-University,
2 Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden
3 Department of Physics, University of California, One Shields Avenue, Davis, CA 95616, USA
Accepted: 11 August 2010
Aims. We present first quantitative results of the surface magnetic field measurements in selected M-dwarfs based on detailed spectra synthesis conducted simultaneously in atomic and molecular lines of the FeH Wing-Ford F4Δ − X4Δ transitions.
Methods. A modified version of the Molecular Zeeman Library (MZL) was used to compute Landé g-factors for FeH lines in different Hund’s cases. Magnetic spectra synthesis was performed with the Synmast code.
Results. We show that the implementation of different Hund’s case for FeH states depending on their quantum numbers allows us to achieve a good fit to the majority of lines in a sunspot spectrum in an automatic regime. Strong magnetic fields are confirmed via the modelling of atomic and FeH lines for three M-dwarfs YZ CMi, EV Lac, and AD Leo, but their mean intensities are found to be systematically lower than previously reported. A much weaker field (1.7–2 kG against 2.7 kG) is required to fit FeH lines in the spectra of GJ 1224.
Conclusions. Our method allows us to measure average magnetic fields in very low-mass stars from polarized radiative transfer. The obtained results indicate that the fields reported in earlier works were probably overestimated by about 15–30%. Higher quality observations are needed for more definite results.
Key words: stars: atmospheres / stars: low-mass / stars: magnetic field
© ESO, 2010
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