THE CENTRAL ENGINES OF TWO UNUSUAL RADIO-INTERMEDIATE/QUIET ACTIVE GALACTIC NUCLEI: III Zw 2 AND PG 1407+265

Chen, Liang; Cao, Xinwu; Bai, J. M.

doi:10.1088/0004-637x/748/2/119

Cited by 23 publications

(25 citation statements)

References 89 publications

(136 reference statements)

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“…Although some groups proposed that the radiation regions of some objects may be outside of the BLR in some states (e.g., Tavecchio et al 2013), some works for an individual source also indicate that the gamma-ray emitting region is inside the BLR (for 3C 279, Bai et al 2009;for 3C 454.3, Isler et al 2013). Since the energy density of torus photon field is much lower than that of BLR, which is about at ∼ 10 −4 erg cm −3 (Ghisellini et al 2008) and the EC process of the BLRs may dominate the IC peaks of the SEDs (e.g., Sikora et al 1994;Ghisellini et al 2009b;Chen et al 2012), we consider only the EC/BLR process. The Klein-Nashina (KN) effects and the absorption of high energy gamma-ray photons by extragalactic background light (Franceschini et al 2008) are also taken into account in our model calculations.…”

Section: Models and Results Of Sed Fits For The Fsrqsmentioning

confidence: 99%

“…The electron distribution is taken as a broken power law as used in the community (Ghisellini et al 2009b;Chen et al 2012;Aharonian et al 2009), which is characterized by an electron density parameter (N 0 ), a break energy γ b and indices (p 1 and p 2 ) in the range of γ e ∼ [γ min , γ max ]. In case of γ e = 1/ 1 − v 2 /c 2 = 1, where v is the velocity of electron, the electron is at rest.…”

Section: Models and Results Of Sed Fits For The Fsrqsmentioning

confidence: 99%

“…It has long been speculated that the physics in different BH jet systems may be essentially the same (Mirabel 2004;Zhang 2007). It is generally believed that jet launching is connected with the central BH, accretion disk and corona in a source (Armitage & Natarajan 1999;Merloni & Fabian 2002;Cao 2004;Wang et al 2004;Chen et al 2012) via either the Blandford-Payne (BP, Blandford & Payne 1982) and/or Blandford-Znajek (BZ, Blandford & Znajek 1977) mechanisms. The BP mechanism may power a jet by releasing the gravitational energy of accreting matter which moves toward the BH.…”

Section: Introductionmentioning

confidence: 99%

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RELATIVISTIC JET PROPERTIES OF GeV-TeV BLAZARS AND POSSIBLE IMPLICATIONS FOR THE JET FORMATION, COMPOSITION, AND CAVITY KINEMATICS

Zhang

Sun

Liang

et al. 2014

ApJ

132

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We fit the spectral energy distributions (SEDs) of a GeV-TeV FSRQ sample with the leptonic model. Their γ min of the relativistic electron distributions, which significantly affect the estimates of the jet properties, are constrained, with a typical value of ∼ 48. Their jet power, magnetized parameter, radiation efficiency, and jet production/radiation rates per central black hole (BH) mass are derived and compared to that of BL Lacs. We show that the FSRQ jets may be dominated by the Poynting flux and have a high radiation efficiency, whereas the BL Lac jets are likely dominated by particles and have a lower radiation efficiency than FSRQs. Being different from BL Lacs, the jet powers of FSRQs are proportional to their central BH masses. The jet production and radiation rates of the FSRQs distribute in narrow ranges and are correlated with each other, whereas no similar feature is found for the BL Lacs. We also show that the jet power is correlated with the cavity kinetic power, and the magnetic field energy in the jets may provide the cavity kinetic energy of FSRQs and the kinetic energy of cold protons in the jets may be crucial for cavity kinetic energy of BL Lacs. We suggest that the dominating formation mechanism of FSRQ jets may be the BZ process, but BL Lac jets may be produced via the BP and/or BZ processes, depending on the structures and accretion rates of accretion disks.

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Section: Models and Results Of Sed Fits For The Fsrqsmentioning

confidence: 99%

Section: Models and Results Of Sed Fits For The Fsrqsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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RELATIVISTIC JET PROPERTIES OF GeV-TeV BLAZARS AND POSSIBLE IMPLICATIONS FOR THE JET FORMATION, COMPOSITION, AND CAVITY KINEMATICS

Zhang

Sun

Liang

et al. 2014

ApJ

132

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“…For the model description, see the Appendix for detail (see also Chen et al 2012;Kang et al 2014). During our modeling, the Doppler beaming factor is assumed to be same as that in Baloković et al (2016), i.e., δ = 25.…”

Section: The Hard X-ray Excess Of Mrk 421mentioning

confidence: 99%

On the Origin of the Hard X-Ray Excess of High-Synchrotron-Peaked BL Lac Object Mrk 421

Chen

2017

ApJ

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For the first time, Kataoka & Stawarz reported a clear detection of a hard X-ray excess, above 20 keV, in the high-synchrotron-peaked BL Lac object Mrk 421. We find that this feature may not be produced by the low-energy part of the same electron population that produced the Fermi/LAT γ-ray. Because of that it is required that the power-law electron energy go down to γ min ≈ 19, which predicts a very strong radio emission (radio flux larger than the observed) even considering the synchrotron self-absorption effect. We investigate the possibility of this excess being produced from the spine/layer jet structure, which has been clearly detected in Mrk 421. We find that (1) similar to one-zone modeling, the spine emissions provide good modeling of the broadband spectral energy distribution, except for the hard X-ray excess; and (2) the hard X-ray excess can be well represented by the synchrotron photons (from the layer) being inverse Compton scattered by the spine electrons.

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“…There are also some analytical works that study the wind from accretion disks (e.g. Li & Cao 2009;Xie et al 2008;Bu et al 2009;Bu & Mosallanezhad 2018;Abbassi et al 2010;Chen et al 2012;Li & Begelman 2014;Gu 2015;Cao 2016). The topic of the wind is interesting because it is now widely believed that AGN feedback plays an important role in the evolution of their host galaxies (e.g., Ciotti & Ostriker 2001, 2007Gan et al 2014;Yuan et al 2018).…”

Section: Discussionmentioning

confidence: 99%

The wind production from black hole hot accretion flow

2018

Proc. IAU

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Observations of low luminosity active galactic nuclei (LLAGNs) and the hard state of black hole X-ray binaries (BHBs) show that the wind exists. Black hole in LLAGNs and hard state of BHBs accretes gas in hot accretion mode. In this paper, we first use magnetohydrodynamic (MHD) simulations of hot accretion flow around a black hole to study the origin of the wind. We find that the wind is driven by the combination of gradients of gas and magnetic pressure and centrifugal forces. Second, we use simulations with focus on the region around Bondi radius to study whether the wind can be generated outside Bondi radius. In the simulation studying hot accretion flow around Bondi radius, in addition to the black hole gravity, we also take into account the gravity of nuclei stars. We find that the wind can not be generated outside Bondi radius. The absence of the wind is due to the change of gravity potential.

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THE CENTRAL ENGINES OF TWO UNUSUAL RADIO-INTERMEDIATE/QUIET ACTIVE GALACTIC NUCLEI: III Zw 2 AND PG 1407+265

Cited by 23 publications

References 89 publications

RELATIVISTIC JET PROPERTIES OF GeV-TeV BLAZARS AND POSSIBLE IMPLICATIONS FOR THE JET FORMATION, COMPOSITION, AND CAVITY KINEMATICS

RELATIVISTIC JET PROPERTIES OF GeV-TeV BLAZARS AND POSSIBLE IMPLICATIONS FOR THE JET FORMATION, COMPOSITION, AND CAVITY KINEMATICS

On the Origin of the Hard X-Ray Excess of High-Synchrotron-Peaked BL Lac Object Mrk 421

The wind production from black hole hot accretion flow

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