X-ray emissions from three-dimensional magnetohydrodynamic coronal accretion flows

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Abstract

Astrophysics with All-Sky X-Ray observations: 3rd International MAXI Workshop (RIKEN, 10-12 June 2008)

In explaining the spectral properties of active galactic nuclei (AGNs) and X-ray binaries, it is often assumed that they consists of a geometrically thin, optically thick disk and hot, optically thin corona surrounding the thin disk. As for a model of a corona, we adopt the simulation data of three-dimensional, non-radiative MHD accretion flows calculated by Kato and coworkers, while for a thin disk we assume a standard type disk. We perform Monte Carlo radiative transfer simulations in the corona, taking into account the Compton scattering of the soft photons from the thin disk by hot thermal electrons and coronal irradiation heating of the thin disk, which emits blacbody radiation. By adjusting the density parameter of the MHD coronal flow, we can produce the emergent spectra which are consistent with those of typical Seyfert galaxies. Moreover, we find rapid time variability in X-ray emission spectra, originating from the density fluctuation produced by the magnetorotational instability in the MHD corona.

資料番号: AA0064306028

レポート番号: JAXA-SP-08-014E

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