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• W336324402 abstract "Abstract. We have measured the equivalent width W K of theKi resonance line at 7699A for a large sample of low activity˚late-type stars observed with high spectral resolution and wehave verified that the relation W K vs. T eff is monotonicallydecreasing, for both dwarf and giant stars. This behaviour isdifferent from that of the NaiD lines for stars of the same type,which showed that the relation W Na vs. T eff has a maximumfor T eff ∼ 4000K, which is better defined for giants than fordwarfs (Tripicchio et al. 1997).The fit of the observed K i equivalent widths by means ofa NLTE spectral line synthesis using conventional backgroundopacity shows that, for dwarf stars, the adopted models overes-timate the observed W K for temperatures <∼ 4000K. This resultis similar to that discussed for the Nai D lines in our previouspaper. On the other hand, for giant stars with T eff <∼ 3800Kthese models in general underestimate W K .ThediscrepanciesbetweenobservedandcomputedW K andW Na for cool stars are much stronger than the variations due touncertainties in either atmospheric model or line parameters,like effective temperature and surface gravity, or Van der Waalsbroadening.ForMdwarfstars,themostconvincingexplanationfor the disagreement is the lack of atomic and molecular lineopacityintheadoptedmodels.Infact,aNLTEspectralsynthesisincluding an additional background opacity reproduces with agood level of accuracy the equivalent widths, as well as thegeneral shape of the profiles for both the Na i D and Ki lines,in a subsample of early-M dwarfs.Key words: stars: late-type – stars: atmospheres – line: forma-tion – radiative transfer – line: profiles1. IntroductionIn a previous work, Tripicchio et al. (1997, hereafter T97) havetested current models of late-type stellar atmospheres (includ-ing photosphere and low chromosphere) using the equivalent" @default.
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• W336324402 date "1999-05-01" @default.
• W336324402 modified "2023-09-28" @default.
• W336324402 title "Probing the {Na} BT I D and {K} BT I lambda 7699 resonance lines sensitivity to background opacity in late-type stars" @default.
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