CaII H+K & MgII h+k line Fluxes from Basal Flux Stars

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The heating mechanisms of the solar chromosphere are still under discussion. Helpful for this topic is to look for basal flux stars that are similar to the Sun.
The minimum observed CaII H+K & MgII h+k line fluxes from stellar Chromospheres as function of effective temperature Teff are called basal flux lines. It is widely thought that these fluxes are caused by non-magnetic heating of the outer stellar atmospheres. We present numerical calculations of basal fluxes for a variety of stars (G0 - K5) of different metallicity and gravity based on self-consistent time-dependent chromospheric models: Assuming purely acoustic heating we theoretically investigate the differences between the basal flux lines of dwarfs, giants and low metallicity stars and compare them with observations. Since basal flux stars rotate very slowly, they are not supposed to be dominated by magnetic fields and therefore their chromospheres should depend only on the three parameters Teff, gravity g and metallicity Z.
Since our acoustic models also depend only on these three parameters, this Comparison could turn out to be a powerful argument for the reality of the acoustic heating picture.

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