Fig. 8 from Power Spectra of Black Holes and Neutron Stars as a Probe of Hydrodynamic Structure of the Source: Diffusion Theory and Its Application to Cygnus X‐1 and Cygnus X‐2 X‐Ray Observations

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Power Spectra of Black Holes and Neutron Stars as a Probe of Hydrodynamic Structure of the Source: Diffusion Theory and Its Application to Cygnus X‐1 and Cygnus X‐2 X‐Ray Observations

Authors: Lev Titarchuk, Nikolai Shaposhnikov, and Vadim Arefiev

Titarchuk, Shaposhnikov, & Arefiev 2007 The Astrophysical Journal 660 556.

Provider: AAS Journals

Caption: Fig. 8.

Cyg X‐1: HF WRN component: the best‐fit diffusion frequency ﹩\nu _{0}=t^{-1}_{0}﹩ vs. Γ (top left), QPO LF ν_QPO (﹩\nu _{L}﹩) vs. Γ (top right), the best‐fit index of the viscosity distribution ψ vs. Γ (bottom left), and inferred Reynolds number Re (using t₀, ν_L, ψ, and eq. [90]) vs. Γ (bottom right).

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