Structure of line-emitting accretion disks in active galactic nuclei - ARP 102B

Chen, Kaiyou; Halpern, J. P.

doi:10.1086/167782

Cited by 240 publications

(188 citation statements)

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“…Objects coming from various subsamples are marked with different symbols but they all form a mostly uniform distribution. The black dot marking an object with a rather large FWHM (15 000 km s −1 ) and low Eddington ratio (0.0022) represents the source Arp 102B (the second to last source from Reference 3 in Table 1), which belongs to the class of radio loud objects with double peaked broad emission lines (Chen & Halpern 1989).…”

Section: Resultsmentioning

confidence: 99%

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Różáńska¹,

Kuraszkiewicz

2004

A&A

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Abstract.We analyze the consequences of the hypothesis that the formation of the Broad Line Region is intrinsically connected to the existence of the cold accretion disk. We assume that the Broad Line Region radius is reliably estimated by the formula of Kaspi et al. (2000, ApJ, 533, 631). We consider three models of the disappearance of the inner disk that limit the existence of the Broad Line Region: (i) the classical ADAF approach, i.e. the inner hot flow develops whenever it can exist; (ii) the disk evaporation model of Meyer & Meyer-Hofmeister (2002, A&A, 392, L5); (iii) the generalized disk evaporation model of Różańska & Czerny (2000b, A&A, 360, 1170. For each of the models, we determine the minimum value of the Eddington ratio and the maximum value of the broad line widths as functions of the viscosity parameter α and the magnetic field parameter β. We compare the predicted parameter space with observations of several AGN. Weak dependence of the maximum value of the FWHM and minimum value of the Eddington ratio on the black hole mass in our sample is noticeable. It seems to favor the description of the cold disk/hot inner flow transition as in the classical ADAF approach rather than with the model of disk evaporation due to conduction between the disk and accreting corona.

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Section: Resultsmentioning

confidence: 99%

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Różáńska¹,

Kuraszkiewicz

2004

A&A

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“…The advectiondominated accretion flow (ADAF) models (Narayan et al 1998), which were successively proposed, follow similar lines of thought. In this picture, the accretion flow in BLRGs could be hot and geometrically thick in the inner regions and become cold and geometrically thin only at larger radii (Chen & Halpern 1989;Grandi et al 1999;Eracleous et al 2000). The weakness …”

Section: Hot Accretion Flowmentioning

confidence: 99%

BeppoSAXView of Radio‐loud Active Galactic Nuclei

Grandi

Malaguti

Fiocchi

2006

ApJ

101

109

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A systematic analysis of a large sample of radio-loud active galactic nuclei (AGNs) available in the BeppoSAX public archive has been performed. The sample includes 3 narrow-line radio galaxies (NLRGs), 10 broad-line radio galaxies (BLRGs), 6 steep-spectrum radio quasars (SSRQs), and 16 flat-spectrum radio quasars (FSRQs). According to the unified models, these classes correspond to objects with increasing viewing angles. As expected, the presence of a nonthermal beamed component emerges clearly in FSRQs. This class shows in fact a featureless continuum (with the exception of 3C 273) and a significantly flatter average spectral slope. However, traces of a nonthermal Doppler-enhanced radiation are elusive in the other classes. We find that the iron line equivalent widths (EWs) are generally weaker in radio-loud AGNs than in Seyfert 1 galaxies, and we confirm the presence of an X-ray Baldwin effect; that is, a decrease of EW with the 2-10 keV luminosity from Seyfert galaxies to BLRGs and quasars. Since the EW-L 2-10 keV anticorrelation is present also in radio-quiet AGNs alone, this effect cannot be ascribed entirely to a strongly beamed jet component. Possible alternative interpretations are explored.

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“…Profiles computed this way have been presented, e.g., by Andy Fabian and collaborators [189] for the Schwarzschild case, and by Chen and Halpern [190] in the weak field limit. In general, however, the computation has to be done in the strong-field Kerr metric.…”

Section: Formalisms For Computing Line Profilesmentioning

confidence: 99%