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Fig. 10

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Volume cooling rates and their most relevant contributors (> 1 % of Ctot at their maximum) calculated for the hot 5 M sub-Neptune under moderate XUV irradiation. The top, middle, and bottom panels present the results of model#1 (pure hydrogen atmosphere), model#3 (hydrogen+helium), and model #5 (solar composition), respectively. The processes responsible for the cooling, and the corresponding line styles are given in the legend located above the top panel with the following notation: Ctot – total volume cooling from all sources; H-line – atomic hydrogen line cooling; free-free H – bremsstrahlung cooling from hydrogen (and helium, when included in the model); H2-molecule – H2 molecule cooling; H2-line (rotation) – line cooling within a H2 molecule; cooling due to recombination of ; H + e → H + hv − cooling due to an electron hitting a hydrogen atom in the ground state loosing its kinetic energy and hydrogen atom can emit a photon; He-line – helium line cooling; C-line – carbon line cooling; Mg-line – magnesium line cooling; Fe-line – iron line cooling. For reference, we include in each panel the advection term including adiabatic cooling from the models with the wind, with the respective composition.

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