Accretion in active galactic nuclei and disk‐jet coupling

You, Bei

doi:10.1002/asna.201512268

Cited by 15 publications

(11 citation statements)

References 122 publications

(112 reference statements)

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“…A, with relatively high L/L Edd (Wu, 2009). Formation of jetted sources may occur also at high Eddington ratio, although the physical mechanism leading to jet production and collimation is presently unclear (for a review, see Czerny and You, 2016), and the jet properties may also be different (Gu, 2017, and references therein). If relatively low power (Komossa et al, 2006).…”

Section: A Bird's Eye View Of the Ms Correlatesmentioning

confidence: 99%

A Main Sequence for Quasars

Marziani

Dultzin

Sulentic

et al. 2018

Front. Astron. Space Sci.

110

123

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The last 25 years saw a major step forward in the analysis of optical and UV spectroscopic data of large quasar samples. Multivariate statistical approaches have led to the definition of systematic trends in observational properties that are the basis of physical and dynamical modeling of quasar structure. We discuss the empirical correlates of the so-called "main sequence" associated with the quasar Eigenvector 1, its governing physical parameters and several implications on our view of the quasar structure, as well as some luminosity effects associated with the virialized component of the line emitting regions. We also briefly discuss quasars in a segment of the main sequence that includes the strongest FeII emitters. These sources show a small dispersion around a well-defined Eddington ratio value, a property which makes them potential Eddington standard candles.

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Section: A Bird's Eye View Of the Ms Correlatesmentioning

confidence: 99%

A Main Sequence for Quasars

Marziani

Dultzin

Sulentic

et al. 2018

Front. Astron. Space Sci.

110

123

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“…If the disk photon enters into the hot flow, it may be Compton scattered by the hot electrons. For simplicity, we assume that the entire hot flow rotates in the radius-dependent Keplerian motion and ignore the radial velocity, although this might not be the case (Czerny & You 2016). The additional component of the flow velocity, due to precession motion, is not taken into account.…”

Section: Spectral State Transitionsmentioning

confidence: 99%

X-Ray Quasi-periodic Oscillations in the Lense–Thirring Precession Model. I. Variability of Relativistic Continuum

You

Bursa

Życki

2018

ApJ

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We develop a Monte Carlo code to compute the Compton-scattered X-ray flux arising from a hot inner flow that undergoes Lense-Thirring precession. The hot flow intercepts seed photons from an outer truncated thin disk. A fraction of the Comptonized photons will illuminate the disk and the reflected/reprocessed photons will contribute to the observed spectrum. The total spectrum, including disk thermal emission, hot flow Comptonization, and disk reflection, is modeled within the framework of general relativity, taking light bending and gravitational redshift into account. The simulations are performed in the context of the Lense-Thirring precession model for the low-frequency quasi-periodic oscillations, so the inner flow is assumed to precess, leading to periodic modulation of the emitted radiation.In this work, we concentrate on the energy-dependent X-ray variability of the model and, in particular, on the evolution of the variability during the spectral transition from hard to soft state, which is implemented by the decrease of the truncation radius of the outer disk towards Innermost Stable Circular Orbit (ISCO). In the hard state, where the Comptonizing flow is geometrically thick, the Comptonization is weakly variable with a fractional variability amplitude of ≤10%; in the soft state, where the Comptonizing flow is cooled down and thus becomes geometrically thin, and the fractional variability of the Comptonization is highly variable, increasing with photon energy. The fractional variability of the reflection increases with energy, and the reflection emission for low spin is counterintuitively more variable than the one for high spin.

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“…Generally, the X-ray emission in radio-quiet AGNs is believed to be produced in the hot corona by the inverse Compton scattering of the soft photons from the accretion disc (e.g., Haardt & Maraschi 1991Liu et al 2002), while the origin of the radio emission in the radio-quiet AGNs is still not fully understood, which is suggested to be from jets by some works although not fully proved (e.g., Czerny & You 2016). It is shown that the study of the relation between the radio luminosity and X-ray luminosity is a very useful tool to investigate the coupling of the accretion and the jet (Merloni et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Exploring the physics of the accretion and jet in nearby narrow-line Seyfert 1 galaxies

Yao

Qiao

et al. 2018

Monthly Notices of the Royal Astronomical Society

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In this paper, we explore the physics of the accretion and jet in narrow-line Seyfert 1 galaxies (NLS1). Specifically, we compile a sample composed of 16 nearby NLS1 with L bol /L Edd 0.1. We investigate the mutual correlation between their radio luminosity L R , X-ray luminosity L X , optical luminosity L 5100 and black hole mass M BH . By adopting partial correlation analysis: (1) we find a positive correlation between L X and M BH , and (2) we find a weak positive correlation between L R and L 5100 . However, we don't find significant correlations between L R and L X or between L X and L 5100 after considering the effect of the black hole mass, which leads to a finding of the independence of L X /L Edd on L 5100 /L Edd . Interestingly, the findings that L X is correlated with M BH and L X /L Edd is not correlated with L 5100 /L Edd support that the X-ray emission is saturated with increasing M for L bol /L Edd 0.1 in NLS1s, which may be understood in the framework of slim disc scenario. Finally, we suggest that a larger NLS1 sample with high quality radio and X-ray data is needed to further confirm this result in the future.

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Accretion in active galactic nuclei and disk‐jet coupling

Cited by 15 publications

References 122 publications

A Main Sequence for Quasars

A Main Sequence for Quasars

X-Ray Quasi-periodic Oscillations in the Lense–Thirring Precession Model. I. Variability of Relativistic Continuum

Exploring the physics of the accretion and jet in nearby narrow-line Seyfert 1 galaxies

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