Spectral line ratios as Teff indicators in solar-like stars

Details Spectral line ratios as Teff indicators in solar-like stars Spectral line ratios as Teff indicators in solar-like stars

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002a%26a...386..286c&link_type=abstract

Astronomy and Astrophysics, v.386, p.286-295 (2002)

Astronomy and Astrophysics

Astrophysics

15

Stars: Late-Type, Stars: Atmosphere, Stars: Fundamental Parameters, Sun: Activity, Convection

Scientific paper

The ratios of spectral line depths are often used as indicators of the stellar effective temperature T_eff. In particular, Gray & Livingston (\cite{grayliv97a}) calibrated the temperature sensitivity of the ratios between the central depths of the line C I 538.032 nm and either the Fe I 537.958 or the Ti II 538.103, making use of observed spectra of several solar-like stars. The ultimate reason for choosing these lines was the subsequent application of their calibration to a long series of solar data, collected at Kitt Peak (in disk-integrated light) from 1978 to 1992, in order to get the T_eff variation of the Sun during its 11-yr magnetic cycle (Gray & Livingston \cite{grayliv97b}). We propose a theoretical calibration that includes a careful treatment of convective transport and fits the stellar data very well , showing, at the same time, that the empirical calibration of Gray and Livingston incorporates in the T_eff sensitivity an undesired dependence of line ratios on the surface gravities of the individual stars they used. A possible dependence of the calibration upon stellar rotation is also explored.

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