Soft X-Ray Excess from Shocked Accreting Plasma in Active Galactic Nuclei

TL;DR

This paper introduces a new model explaining the soft X-ray excess in Seyfert galaxies as Comptonization of disk photons by shock-heated plasma near black holes, supported by spectral fitting of AGN data.

Contribution

The study develops a relativistic MHD shock model for accreting plasma and demonstrates its ability to reproduce observed X-ray spectra in Seyfert galaxies.

Findings

Model successfully fits X-ray spectra of Ark 120.

Derived electron temperatures range from 61.3 keV to 144.3 keV.

The Comptonizing region is compact, about 3-4 gravitational radii.

Abstract

We propose a novel theoretical model to describe a physical identity of the soft X-ray excess, ubiquitously detected in many Seyfert galaxies, by considering a steady-state, axisymmetric plasma accretion within the innermost stable circular orbit (ISCO) around a black hole (BH) accretion disk. We extend our earlier theoretical investigations on general relativistic magnetohydrodynamic (GRMHD) accretion which has implied that the accreting plasma can develop into a standing shock for suitable physical conditions causing the downstream flow to be sufficiently hot due to shock compression. We numerically calculate to examine, for sets of fiducial plasma parameters, a physical nature of fast MHD shocks under strong gravity for different BH spins. We show that thermal seed photons from the standard accretion disk can be effectively Compton up-scattered by the energized sub-relativistic electrons in the hot downstream plasma to produce the soft excess feature in X-rays. As a case study, we construct a three-parameter Comptonization model of inclination angle $\theta_{\rm obs}$, disk photon temperature $kT_{\rm in}$ and downstream electron energy $kT_e$ to calculate the predicted spectra in comparison with a 60 ks {\it XMM-Newton}/EPIC-pn spectrum of a typical radio-quiet Seyfert 1 AGN, Ark~120. Our $\chi^2$-analyses demonstrate that the model is plausible in successfully describing data for both non-spinning and spinning BHs with the derived range of $61.3~{\rm keV} \lesssim kT_e \lesssim 144.3~{\rm keV}$, $21.6~{\rm eV} \lesssim kT_{\rm in} \lesssim 34.0~{\rm eV}$ and $17.5\degr \lesssim \theta_{\rm obs} \lesssim 42.6\degr$ indicating a compact Comptonizing region of $3-4$ gravitational radii that resembles the putative X-ray coronae.