The jets-accretion relation, mass-luminosity relation in Fermi blazars

Yu, Xiaoling; Zhang, Xiong; Zhang, Haojing; Xiong, Dingrong; Li, Bijun; Cha, Yongjuan; Chen, Yongyun; Huang, Xia; Wang, Yuwei

doi:10.1007/s10509-015-2309-4

Cited by 11 publications

(7 citation statements)

References 68 publications

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“…From this plot, we notice that the baryonic loading obtained is compatible with the Eddington luminosity for the Lorentz factor and the black hole masses that we have discussed. Note that the quantity L edd may also vary with L γ , due to the fact that the black hole mass and the ejected luminosity are slightly correlated, as found in Yu et al (2015). On the other hand, this behavior is contained in the uncertainties that we have used, i.e., within the red region in the left panel of Fig.…”

Section: Source Parameters With γ-Ray Luminositymentioning

confidence: 74%

“…A range of supermassive black hole masses of M ∈ [10 7.5 , 10 9.5 ]M is assumed, which is typical for blazars (Ghisellini & Tavecchio (2008); Ghisellini et al (2010), see also Fig. 7 of Yu et al (2015)). Note that the Eddington luminosity is not a hard limit on the expected luminosity of blazars and may be exceeded, especially during flares (Sadowski & Narayan 2015).…”

Section: Source Parameters With γ-Ray Luminositymentioning

confidence: 99%

See 1 more Smart Citation

Interpretation of the Diffuse Astrophysical Neutrino Flux in Terms of the Blazar Sequence

Palladino¹,

Rodrigues²,

Gao³

et al. 2019

ApJ

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We study if the diffuse astrophysical neutrino flux can come from blazar jets -a subclass of Active Galactic Nuclei (AGNs) -while it, at the same time, respects the blazar stacking limit based on source catalogs and is consistent with the observation from TXS 0506+056. We compute the neutrino flux from resolved and unresolved sources using an averaged, empirical relationship between electromagnetic spectrum and luminosity, known as the blazar sequence, for two populations of blazars (BL Lacs and FSRQs). Using a source model with realistic neutrino flux computations, we demonstrate that blazars can indeed power the diffuse neutrino flux at the highest energies and obey the stacking limit at the same time, and we derive the conditions for the baryonic loading (proton versus γ-ray luminosity) evolving over the blazar sequence. Under the hypothesis that low-luminosity blazars power the diffuse astrophysical neutrino flux, we find that the dominant contribution of the diffuse flux up to PeV energies must come from unresolved BL Lacs with baryonic loadings larger than about 10 5 -while only a very small contribution may come from resolved high-luminosity BL Lacs or FSRQs, which can be directly tested by the stacking limit. We find that the blazar TXS 0506+056 is on the verge of these populations in our baseline scenario, at a relatively high luminosity and redshift; as a consequence we predict about 0.3 γ-ray-neutrino associations per year from the whole population, dominated by BL Lacs with L γ 10 45 erg/s and z ∼ 0.1. arXiv:1806.04769v4 [astro-ph.HE]

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Section: Source Parameters With γ-Ray Luminositymentioning

confidence: 74%

Section: Source Parameters With γ-Ray Luminositymentioning

confidence: 99%

Interpretation of the Diffuse Astrophysical Neutrino Flux in Terms of the Blazar Sequence

Palladino¹,

Rodrigues²,

Gao³

et al. 2019

ApJ

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“…In this sense we may talk about an environmental astrophysics. Evidences of this fact are the debates on the jet-accretion correlation, the BH accretion rate-disk luminosity issue, the BH growth-accretion disk and BH-spin shift-accretion disk correlation and BH populations and galaxy age correlation-see for example Madau (1988), Volonteri et al (2003a), Narayan and McClintock (2013), Morningstar et al (2014), Yu et al (2015), Mewes et al (2016), Sadowski et al (2016), Hirano et al (2017), Lee et al (2017b), Regan et al (2017), Ricci et al (2017b), Xie and Yuan (2017) and Yang et al (2017).…”

Section: Introductionmentioning

confidence: 99%

“…Quantum Grav. 35 (2018) 185008 Marscher et al (2002), Maraschi and Tavecchio (2003), Maitra et al (2009), Ghisellini et al (2014), Sbarrato et al (2014), Chen et al (2015), Yu et al (2015) and Zhang et al (2015). For jet-accretion disk correlation in AGN see for example Banados et al (2017), Bogdan et al (2017), Caproni et al (2017), D'Ammando (2017), Duran et al (2017), Gandhi et al (2017), Inoue et al (2017), Vedantham et al (2017) and Liska et al (2018) and also Fender and Belloni (2004), Fender (2009), Neilsen and Lee (2009), Soleri et al (2010), Toba et al (2017), Fang and Murase (2018) and Tetarenko et al (2018).…”

Section: Introductionmentioning

confidence: 99%

Relating Kerr SMBHs in active galactic nuclei to RADs configurations

Pugliese

Stuchlík

2018

Class. Quantum Grav.

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There is strong observational evidence that many active galactic nuclei (AGNs) harbour supermassive black holes (SMBHs), demonstrating multi-accretion episodes during their life-time. In such AGNs, corotating and counterrotating tori, or strongly misaligned disks, as related to the central Kerr SMBH spin, can report traces of the AGNs evolution. Here we concentrate on aggregates of accretion disks structures, ringed accretion disks (RADs) orbiting a central Kerr SMBH, assuming that each torus of the RADs is centered in the equatorial plane of the attractor, tori are coplanar and axi-symmetric. Many of the RAD aspects are governed mostly by the spin of the Kerr geometry. We classify Kerr black holes (BHs) due to their dimensionless spin, according to possible combinations of corotating and counterrotating equilibrium or unstable (accreting) tori composing the RADs. The number of accreting tori in RADs cannot exceed n = 2. We present list of 14 characteristic values of the Kerr BH dimensionless spin a governing the classification in whole the black hole range 0 ≤ a ≤ M , uniquely constrained by the RAD properties. The spin values are remarkably close providing an accurate characterization of the Kerr attractors based on the RAD properties. RAD dynamics is richer in the spacetimes of high spin values. One of the critical predictions states that a RAD tori couple formed by an outer accreting corotating and an inner accreting counterrotating torus is expected to be observed only around slowly spinning (a < 0.46M ) BHs. The analysis strongly binds the fluid and BH characteristics providing indications on the situations where to search for RADs observational evidences. Obscuring and screening tori, possibly evident as traces in X-ray spectrum emission, are strongly constrained, eventually ruling out many assumptions used in the current investigations of the screening effects.We expect relevance of our classification of Kerr spacetimes in relation to astrophysical phenomena arising in different stages of AGNs life that could be observed by the planned X-ray satellite observatory ATHENA (Advanced Telescope for High ENergy Astrophysics).

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“…In this regard the investigation is increasingly directed to find correlations between different phenomena framed in the BH-disk system: for example in the BH populations and galaxy age correlation and BH-spin shift-accretion disk correlation and in the jet-accretion correlation-see for example [19][20][21][22][23][24][25][26][27][28][29][30][31]. The BH spin variation follows BH interaction with its environment, therefore many approaches in the evaluation of the BHs parameters and estimation of BH accretion history are connected to the accretion disk physics, based for example on the evaluation of the disk luminosity or accretion rates.…”

Section: Introductionmentioning

confidence: 99%

General relativistic rotational energy extraction from black holes-accretion disk systems

Pugliese

Stuchlík

2021

Class. Quantum Grav.

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The determination of mass and spin parameters of the black holes (BHs) is crucial in the analysis of the merger of BHs and BHs formation and evolution, including accretion. Here we constrain the BH spin with the evaluation of the dimensionless parameter ξ representing the total rotational energy extracted versus the mass of the BH, following procedure introduced by Daly (2009 Astrophys. J. 691 L72–6) that is independent from the details of the specific extraction process. The energy extraction can power an outflow which can be then observed. We relate the energy extraction to the accreting configurations and the accretion processes occurring in a cluster of agglomerate corotating and counter-rotating tori orbiting one central Kerr SMBH, associating ξ to the characteristics of the accretion processes. We relate the regions of tori parameters to features of the energy extraction processes, binding ξ to properties of light surfaces by using the bundles developed by Pugliese and Quevedo (2019 Eur. Phys. J. C 79 209), relating measures in different regions of the spacetimes. We evaluate properties of the BH accretions disks, and correlate spacetimes prior and after their transition due to the energy extraction. Light surfaces are related to the generators of Killing horizons, proving limiting frequency of the stationary observers of the geometries. We consider the photon limiting curves of the stationary observers as constraints for various processes regulated by these frequencies, to relate different BH states, prior and after the energy extraction, investigating regions close to the BH horizons and rotational axis. From methodological view-point we used a naked singularity—BH correspondence defined with metric bundles to predict observational characteristics of the BH—accretion disk system. The analysis points relevant BH spins a ≈ 0.94M, a ≈ 0.7M and a ≈ 0.3M. We show the relation between the rotational law of the tori, the characteristic frequency of the bundle and the relativistic velocity defining the von Zeipel surfaces. The inferior limit on the formation of corotating tori is ℓ/a ⩾ 2, for counter-rotating tori ℓ/a ⩽ −22/5 (ℓ is the fluids specific angular momentum).

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The jets-accretion relation, mass-luminosity relation in Fermi blazars

Cited by 11 publications

References 68 publications

Interpretation of the Diffuse Astrophysical Neutrino Flux in Terms of the Blazar Sequence

Interpretation of the Diffuse Astrophysical Neutrino Flux in Terms of the Blazar Sequence

Relating Kerr SMBHs in active galactic nuclei to RADs configurations

General relativistic rotational energy extraction from black holes-accretion disk systems

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