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Fig. 10


Heating rate (top panel) and cooling rate (bottom panel) of the photoionised gas in NGC 7469 as a function of the ionisation parameter ξ. The contributions by the main processes to the total rates (shown by solid lines) are individually shown. Heating by Compton scattering (long-dashed lines), photoelectrons (dashed lines), and Auger electrons (dotted lines) are displayed in the top panel. Cooling by inverse Compton scattering (long-dashed lines), Bremsstrahlung (dashed lines), collisional excitation (dotted lines), and recombination (dashed-dotted lines) are displayed in the bottom panel. The curves are calculated for the 2002 and 2015 SEDs (Fig. 2, bottom panel). The thick stripes on each curve indicate the position of the derived wind absorption components (Comps. A to D) from the best-fit model to the 2002 and 2015 HETGS spectra. For identification, Comp. A has the lowest ξ and Comp. D the highest.

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