Radiation MHD Simulations of Soft X-ray Emitting Regions in Changing Look AGN
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2024
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| author | Igarashi, Taichi Takahashi, Hiroyuki R. Kawashima, Tomohisa Ohsuga, Ken Matsumoto, Yosuke Matsumoto, Ryoji |
| author_facet | Igarashi, Taichi Takahashi, Hiroyuki R. Kawashima, Tomohisa Ohsuga, Ken Matsumoto, Yosuke Matsumoto, Ryoji |
| contents | Strong soft X-ray emission called soft X-ray excess is often observed in luminous active galactic nuclei (AGN). It has been suggested that the soft X-rays are emitted from a warm ($T=10^6\sim10^7\ \rm{K}$) region that is optically thick for the Thomson scattering (warm Comptonization region). Motivated by the recent observations that soft X-ray excess appears in changing look AGN (CLAGN) during the state transition from a dim state without broad emission lines to a bright state with broad emission lines, we performed global three-dimensional radiation magnetohydrodynamic simulations assuming that the mass accretion rate increases and becomes around $10$\% of the Eddington accretion rate. The simulation successfully reproduces a warm, Thomson-thick region outside the hot radiatively inefficient accretion flow near the black hole. The warm region is formed by efficient radiative cooling due to inverse Compton scattering. The calculated luminosity $0.01L_{\rm Edd}-0.08L_{\rm Edd}$ is consistent with the luminosity of CLAGN. We also found that the warm Comptonization region is well described by the steady model of magnetized disks supported by azimuthal magnetic fields. When the anti-parallel azimuthal magnetic fields supporting the radiatively cooled region reconnect around the equatorial plane of the disk, the temperature of the region becomes higher by releasing the magnetic energy transported to the region. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2407_01876 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Radiation MHD Simulations of Soft X-ray Emitting Regions in Changing Look AGN Igarashi, Taichi Takahashi, Hiroyuki R. Kawashima, Tomohisa Ohsuga, Ken Matsumoto, Yosuke Matsumoto, Ryoji High Energy Astrophysical Phenomena Astrophysics of Galaxies Strong soft X-ray emission called soft X-ray excess is often observed in luminous active galactic nuclei (AGN). It has been suggested that the soft X-rays are emitted from a warm ($T=10^6\sim10^7\ \rm{K}$) region that is optically thick for the Thomson scattering (warm Comptonization region). Motivated by the recent observations that soft X-ray excess appears in changing look AGN (CLAGN) during the state transition from a dim state without broad emission lines to a bright state with broad emission lines, we performed global three-dimensional radiation magnetohydrodynamic simulations assuming that the mass accretion rate increases and becomes around $10$\% of the Eddington accretion rate. The simulation successfully reproduces a warm, Thomson-thick region outside the hot radiatively inefficient accretion flow near the black hole. The warm region is formed by efficient radiative cooling due to inverse Compton scattering. The calculated luminosity $0.01L_{\rm Edd}-0.08L_{\rm Edd}$ is consistent with the luminosity of CLAGN. We also found that the warm Comptonization region is well described by the steady model of magnetized disks supported by azimuthal magnetic fields. When the anti-parallel azimuthal magnetic fields supporting the radiatively cooled region reconnect around the equatorial plane of the disk, the temperature of the region becomes higher by releasing the magnetic energy transported to the region. |
| title | Radiation MHD Simulations of Soft X-ray Emitting Regions in Changing Look AGN |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.01876 |