Chromospheric Activity in 55 Cancri: Ii. Theoretical Wave Studies Versus Observations

Abstract

In this study, we consider chromospheric heating models for 55 Cancri in conjunction with observations. The theoretical models, previously discussed in , are self-consistent, non-linear, and time-dependent ab-initio computations encompassing the generation, propagation, and dissipation of waves. Our focus is the consideration of both acoustic waves and longitudinal flux tube waves amounting to two-component chromosphere models. 55 Cancri, a K-type orange dwarf, is a star of low activity, as expected by its age, which also implies a relatively small magnetic filling factor. The Caii K fluxes are computed (multi-ray treatment) assuming partial redistribution and time-dependent ionization. The theoretical Caii H+K fluxes are subsequently compared with observations. It is found that for stages of lowest chromospheric activity the observed Caii fluxes are akin, though not identical, to those obtained by acoustic heating, but agreement can be obtained if low levels of magnetic heating - consistent with the expected photospheric magnetic filling factor - are considered as an additional component; this idea is in alignment with previous proposals conveyed in the literature.