A New Technique for the Measurement of Stellar Magnetic Fields: First Results
A technique for determining strengths and filling factors of stellar magnetic fields is presented. It is based on a statistical analysis of a large number of unblended Fe I lines and was first introduced by Stenflo and Lindegren (1977). It has been tested in solar active regions and is now applied to late type stars. First results of an analysis of high S/N spectra of three stars are presented and compared to previous measurements. One advantage of the method is that unlike the often used Robinson technique (Robinson, 1980) it is relatively insensitive to the presence of small blends. Finally, the statistical method in principle allows us to decide whether the observed field is concentrated in stellar spots or in plages. Preliminary results for HR 1084 suggest that the field is in the form of plages.
KeywordsFilling Factor Zeeman Splitting Solar Active Region Solar Data Late Type Star
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