SPECTRA MODELLING
work (in progress) of
Iris Bermejo Lozano, Colin P. Folsom,
Gregg A. Wade &
Daniela Korčáková
We use the ZEEMAN code for the spectral modelling (
Landstreet, 1988;
Wade et al., 2001;
Folsom et al., 2012).
This code includes magnetic field in the LTE radiative transfer through the atmosphere.
small insidiousness
-
The strong magnetic field complicates the precise determination of the stellar parameters. For example, the problematic
is even
The fitting of standard synthetic spectra takes the line broadening due to the Zeeman effect as the broadening
due to the rotation. Obtained values are therefore overestimated.