Zeeman Broadening in Cool Stars

Details Zeeman Broadening in Cool Stars Zeeman Broadening in Cool Stars

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..708a&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Spectroscopy And Spectrophotometry, Magnetic And Electric Fields, Polarization Of Starlight, Extrasolar Planetary Systems, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation

Scientific paper

We investigate detectability of magnetic fields by Zeeman broadening of well-isolated spectral lines in F, G and K type stars. Data of unprecedented quality were taken with CES1 mounted on the 3.6 m ESO telescope at La Silla, Chile, in three campaigns in the optical range between 5770 Å and 6280 Å, each with a wavelength coverage of roughly 40 Å. We use the SPINOR/STOPRO (cf. Frutiger et al. [1]) package developed by ETH2 and MPS3 to perform spectral line inversion via χ2 minimization. Starting from constraints given by previous measurements of stellar parameters, we fit a number of extracted spectral lines. Eventually, our goal is to determine the product of the magnetic field strength B and the surface filling factor, B×f.
Our work is in progress and thus no final measurements can be presented at this stage.

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