Fe I lines in spectra of cool stars: temperature diagnostic of the solar-like atmosphere.

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Stellar Atmospheres: Iron Lines, Stellar Atmospheres: Non-Lte Analysis, Solar Atmosphere: Iron Lines, Cool Stars: Iron Lines

Scientific paper

NLTE modelling of Fe I lines is employed with a comprehensive atomic models and for a few models of solar-like atmosphere. Errors that arise in LTE inversion of these lines to recover temperature of the atmosphere are estimated. The temperature uncertainties due to the neglect of NLTE effects in the Fe I lines depend on the line formation height and on the excitation potential of the lower level EPL as a parameter. The errors might reach a few hundred degrees for the photospheric lines and thousand degrees for the chromospheric ones. LTE inversion techniques generally lead to structures with temperature monotonically decreasing outside while there are appreciable differences between structures recovered using various EPL classes of the Fe I lines. Among all these lines three subclasses are selected for whom the LTE assumption masks the NLTE effects in the same structure. The latter turns out to be a HOLMUL-like if the "real Sun" is close to the MACKKL model.

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