Broad-Band Spectral Energy Distributions of Active Galactic Nuclei from an Accretion Disk with Advective Coronal Flow

Details Broad-Band Spectral Energy Distributions of Active Galactic Nuclei from an Accretion Disk with Advective Coronal Flow Broad-Band Spectral Energy Distributions of Active Galactic Nuclei from an Accretion Disk with Advective Coronal Flow

2000-08-25

arxiv.org/abs/astro-ph/0008404v1

Astronomy and Astrophysics

Astrophysics

12 pages, 9 figures, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/318297

We construct a disk-corona model which accounts for the optical-to-X-ray spectral properties of Seyfert nuclei and QSOs. We study emission spectrum emerging from a vertical disk-corona structure composed of two-temperature plasma by solving hydrostatic equilibrium and radiative transfer self-consistently. A fraction $f$ of viscous heating is assumed to be dissipated in a corona with a Thomson optical depth of $\tau_c$, where advective cooling is also included, and a remaining fraction, $1-f$, dissipates within a main body of the disk. Our model can nicely reproduce the soft X-ray excess with a power-law shape and the hard tail extending to $\sim$ 50 keV. The different spectral slopes ($\alpha \sim$ 1.5 below 2keV and $\sim$ 0.5 above, where $\Fnu \propto \nu^{- \alpha}$) are the results of different emission mechanisms and different sites; the former slope is due to unsaturated Comptonization from the innermost zone and the latter is due to a combination of the Comptonization, bremsstrahlung and a reflection of the coronal radiation at the disk-corona boundary from the inner to surrounding zone ($\leq$ 300 Schwarzschild radii). The emergent optical spectrum is redder ($\alpha \sim 0.3$) than that of the standard disk ($\alpha \sim -0.3$), being consistent with observations, due to the different efficiencies of spectral distortion of disk emission at different radii. Further, we find that the cut-off frequency of the hard X-ray ($\sim$ coronal electron temperature) and broad-band spectral shape are insensitive to the black-hole mass, while the peak frequency of the big blue bump is sensitive to the mass as the peak frequency $\propto \Mbh^{-1/4}$.

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