Investigation of stellar magnetic fields based on the strengths of spectral lines - Application to Omicron Pegasi and Cool AP Stars

Details Investigation of stellar magnetic fields based on the strengths of spectral lines - Application to Omicron Pegasi and Cool AP Stars Investigation of stellar magnetic fields based on the strengths of spectral lines - Application to Omicron Pegasi and Cool AP Stars

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..453t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 45, no. 3, p. 453-469.

Other

8

A Stars, Cool Stars, Field Strength, Peculiar Stars, Stellar Atmospheres, Stellar Magnetic Fields, Abundance, Spectral Line Width, Zeeman Effect

Scientific paper

A practical method for simultaneous determinations of H (magnetic field) and xi (microturbulence) in a stellar atmosphere is presented, which is based on the requirement that the scatter of the abundances derived from individual lines should be minimized for the best choice of H and xi. This procedure may be regarded as being an improved and extended version of the classical Hensberge-De Loore method, since it is based on a 'fine analysis' technique using a model atmosphere and the detailed Zeeman-split components of a line are explicitly taken into account with an approximate treatment of the polarization effect. This method was first applied to the hot Am star O Peg, resulting in H = 2 kG (and xi is about 1.5 km/s); this H value is fairly consistent with other estimates based either on the Stenflo-Lindegren technique or on the line-pair method. As an alternative application, surface magnetic fields of five cool Ap stars were also investigated, showing that the H-values by this method agree well with those derived from the method of differential Zeeman broadening and that the classical Hensberge-De Loore technique tends to yield somewhat underestimated values.

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