Table 3.
Average formation heights of the investigated spectral lines.
| Line | Ca II K | Ca II H | He I D3 | Hα | Hβ | NaD2 | Mg I | NaD1 | Ca I 6162 | Fe I 6301 | Fe I 6173 | C I 5380 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Formation | 2200 | 2080 | 2000 | 1300 | 1200 | 968 | 910 | 888 | 495 | 314 | 100 | 40 |
| Height [km] |
Notes. Ca II H & K: Bjørgen et al. (2018), He I D3: de la Cruz Rodríguez et al. (2019), Hα & Hβ: Capparelli et al. (2017), NaD1 & NaD2: Bommier (2016), Mg I & Ca I: Sampoorna & Nagendra (2017), Fe I 6301 Å: Grec et al. (2010), Fe I 6173 Å: Fleck et al. (2011), C I: Joshi et al. (2011). It is important to note that the formation heights provided here are intended to provide a general guide for the readers. Activity and structure variations impact the line formation heights, but will not vary so much that a chromospheric line like Hα to form at a lower height than a photospheric line like Fe I 6173 Å. These variations typically preserve the height ordering presented.
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