The Physical Mechanism of Radio-quiet Turn-on Changing-look Active Galactic Nuclei
It is suggested that the variation of the mass accretion rate in the accretion disk may be responsible for the occurrence of most changing-look active galactic nuclei (CL AGNs). However, the viscous timescale of a thin disk is far longer than the observed timescale of CL AGNs. Though this problem ca...
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| Published in: | The Astrophysical journal Vol. 988; no. 2; pp. 207 - 213 |
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| Language: | English |
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| Abstract | It is suggested that the variation of the mass accretion rate in the accretion disk may be responsible for the occurrence of most changing-look active galactic nuclei (CL AGNs). However, the viscous timescale of a thin disk is far longer than the observed timescale of CL AGNs. Though this problem can be resolved by introducing the large-scale magnetic field, the mechanism for radio-quiet CL AGNs with a weak/absent large-scale magnetic field remains a mystery. In this work, we assume that the thin accretion disk is collapsed from the inner advection-dominated accretion flow (ADAF) instead of being formed from the outer thin disk through advection. This idea is tested by comparing the cooling timescale ( t cool ) of an ADAF with the observed timescale ( t tran ) of turn-on CL AGNs. We compile a sample of 102 turn-on CL AGNs from the archived data and calculate the cooling timescale of an ADAF with the critical mass accretion rate based on some conventional assumptions. It is found that t cool is much shorter than t tran in most of the CL AGNs, which validates our assumption, though t cool is not consistent with t tran ( t cool < t tran ). However, this is reasonable since most of the CL AGNs were observed only two times, indicating that the observed timescale t tran is the maximum value because the changing-look behavior can indeed happen before the second observation. |
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| AbstractList | It is suggested that the variation of the mass accretion rate in the accretion disk may be responsible for the occurrence of most changing-look active galactic nuclei (CL AGNs). However, the viscous timescale of a thin disk is far longer than the observed timescale of CL AGNs. Though this problem can be resolved by introducing the large-scale magnetic field, the mechanism for radio-quiet CL AGNs with a weak/absent large-scale magnetic field remains a mystery. In this work, we assume that the thin accretion disk is collapsed from the inner advection-dominated accretion flow (ADAF) instead of being formed from the outer thin disk through advection. This idea is tested by comparing the cooling timescale (tcool) of an ADAF with the observed timescale (ttran) of turn-on CL AGNs. We compile a sample of 102 turn-on CL AGNs from the archived data and calculate the cooling timescale of an ADAF with the critical mass accretion rate based on some conventional assumptions. It is found that tcool is much shorter than ttran in most of the CL AGNs, which validates our assumption, though tcool is not consistent with ttran (tcool < ttran). However, this is reasonable since most of the CL AGNs were observed only two times, indicating that the observed timescale ttran is the maximum value because the changing-look behavior can indeed happen before the second observation. It is suggested that the variation of the mass accretion rate in the accretion disk may be responsible for the occurrence of most changing-look active galactic nuclei (CL AGNs). However, the viscous timescale of a thin disk is far longer than the observed timescale of CL AGNs. Though this problem can be resolved by introducing the large-scale magnetic field, the mechanism for radio-quiet CL AGNs with a weak/absent large-scale magnetic field remains a mystery. In this work, we assume that the thin accretion disk is collapsed from the inner advection-dominated accretion flow (ADAF) instead of being formed from the outer thin disk through advection. This idea is tested by comparing the cooling timescale ( t cool ) of an ADAF with the observed timescale ( t tran ) of turn-on CL AGNs. We compile a sample of 102 turn-on CL AGNs from the archived data and calculate the cooling timescale of an ADAF with the critical mass accretion rate based on some conventional assumptions. It is found that t cool is much shorter than t tran in most of the CL AGNs, which validates our assumption, though t cool is not consistent with t tran ( t cool < t tran ). However, this is reasonable since most of the CL AGNs were observed only two times, indicating that the observed timescale t tran is the maximum value because the changing-look behavior can indeed happen before the second observation. |
| Author | Cao, Xinwu Li, Shuang-Liang |
| Author_xml | – sequence: 1 givenname: Shuang-Liang orcidid: 0000-0002-7299-4513 surname: Li fullname: Li, Shuang-Liang organization: Chinese Academy of Sciences Shanghai Astronomical Observatory, 80 Nandan Road, Shanghai 200030, lisl@shao.ac.cn People’s Republic of China – sequence: 2 givenname: Xinwu orcidid: 0000-0002-2355-3498 surname: Cao fullname: Cao, Xinwu organization: Zhejiang University Institute for Astronomy, School of Physics, 866 Yuhangtang Road, Hangzhou 310058, xwcao@zju.edu.cn People’s Republic of China |
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| SubjectTerms | Accretion Accretion disks Active galactic nuclei Advection Black hole physics Magnetic fields Time |
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| Title | The Physical Mechanism of Radio-quiet Turn-on Changing-look Active Galactic Nuclei |
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