Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431..844b&link_type=abstract
The Astrophysical Journal, vol. 431, no. 2, pt. 1, p. 844-849
Astronomy and Astrophysics
Astrophysics
23
Dwarf Stars, K Stars, Line Spectra, Stellar Atmospheres, Stellar Magnetic Fields, Zeeman Effect, Astronomical Spectroscopy, Cosmology, Radiative Transfer, Spectrum Analysis, Stellar Spectra
Scientific paper
We have searched for the predicted enhancement of the equivalent widths of Zeeman-sensitive lines in five chromospherically active K dwarfs, by direct comparison with inactive dwarfs of similar spectral type. In two active stars, EQ Vir and HD 82558, the equivalent widths indeed exhibit enhancements (of up to 30%) which correlate with the Zeeman sensitivity of the individual lines. HD 17925 barely shows the effect, and epsilon Eri does not show it. The amount of the Zeeman effect is related to the enhancement of the emission cores of the Ca II infrared triplet lines. Radiative transfer models including magnetic fields permit estimates of Bf, the product of field strength (B) and surface filling factor (f). Our detections imply Bf approximately equals 2kG to 3kG, in agreement with Saar. Difficulties in predicting line strengths from active stars arise due to surface inhomogeneities. These render the method ineffective in our most active case, GI 171.2.
Basri Gibor
Marcy Geoffrey W.
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