EXOSAT‐ASM‐PCA (RXTE) power spectrum of Cyg X‐2 in frequency range that covers 10 orders of magnitude. One can clearly see LF and HF WRN components in PDS, related to the extended Keplerian disk and relatively compact, inner disklike configuration (sub‐Keplerian Compton corona), respectively. Each of these two components is perfectly fitted by our WRN model (see eqs. [85] and [86]); dotted and solid lines are for LF and HF best‐fit models, respectively, with ﹩\chi ^{2}/ N_{\mathrm{dof}\,}=393.2/ 244=1.6﹩ (see the text for the best‐fit parameter values).