Chromospheric activity in 55 Cancri - I. Results from theoretical wave studies

We present theoretical models of chromospheric heating for 55 Cancri, an orange dwarf of relatively low activity. Self-consistent, non-linear, and time-dependent ab initio numerical computations are pursued encompassing the generation, propagation, and dissipation of waves. We consider longitudinal waves operating among arrays of flux tubes as well as acoustic waves pertaining to non-magnetic stellar regions. Additionally, flux enhancements for the longitudinal waves are also taken into account as supplied by transverse tube waves. The Caii K fluxes are computed (multi-ray treatment) assuming partial redistribution as well as time-dependent ionization (TDI). The self-consistent treatment of TDI (especially for hydrogen) greatly impacts the atmospheric temperatures and electron densities (especially behind the shocks); it also affects the emergent Ca ii fluxes. Particularly, we focus on the influence of magnetic heating on the stellar atmospheric structure and the emergent Caii emission, as well as the impact of non-linearities. Our study shows that a higher photospheric magnetic filling factor entails a larger Caii emission; however, an increased initial wave energy flux (e.g. associated with mode coupling) is of little difference. Comparisons of our theoretical results with observations will be conveyed in forthcoming Paper II.

Automated summary

We present theoretical models of chromospheric heating for 55 Cancri, focusing on the impact of longitudinal waves and acoustic waves on the Caii K fluxes. Our study explores the influence of magnetic heating on the stellar atmospheric structure and the emergent Caii emission, as well as the effects of non-linearities, showing that a higher photospheric magnetic filling factor leads to a larger Caii emission. Comparisons with observations will be discussed in forthcoming Paper II.