X-ray Reflection By Photoionized Accretion Discs

Details X-ray Reflection By Photoionized Accretion Discs X-ray Reflection By Photoionized Accretion Discs

2001-02-02

arxiv.org/abs/astro-ph/0102040v2

Mon.Not.Roy.Astron.Soc.327:10,2001

Astronomy and Astrophysics

Astrophysics

16 pages, accepted by MNRAS, Fig. 8 is in colour Figures and tables changed by a code update. Conclusions unchanged

Scientific paper

10.1046/j.1365-8711.2001.04432.x

We present the results of reflection calculations that treat the relevant physics with a minimum of assumptions. The temperature and ionization structure of the top five Thomson depths of an illuminated disc are calculated while also demanding that the atmosphere is in hydrostatic equilibrium. In agreement with Nayakshin, Kazanas & Kallman, we find that there is a rapid transition from hot to cold material in the illuminated layer. However, the transition is usually not sharp so that often we find a small but finite region in Thomson depth where there is a stable temperature zone at T \sim 2 x 10^{6} K due to photoelectric heating from recombining ions. As a result, the reflection spectra often exhibit strong features from partially-ionized material, including helium-like Fe K lines and edges. We find that due to the highly ionized features in the spectra these models have difficulty correctly parameterizing the new reflection spectra. There is evidence for a spurious $R-\Gamma$ correlation in the ASCA energy range, where $R$ is the reflection fraction for a power-law continuum of index $\Gamma$, confirming the suggestion of Done & Nayakshin that at least part of the R-Gamma correlation reported by Zdziarski, Lubinski & Smith for Seyfert galaxies and X-ray binaries might be due to ionization effects. Although many of the reflection spectra show strong ionized features, these are not typically observed in most Seyfert and quasar X-ray spectra.

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