An Analysis of the Synchrotron Self-Compton Model for the Multi--Wave Band Spectra of Blazars

Bloom, S. D.; Marscher, A. P.

doi:10.1086/177092

Cited by 471 publications

(395 citation statements)

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“…The low energy component is generally attributed to synchrotron radiation from electrons and positrons in the knots moving at relativistic speed in the jet. The high energy component can have different origins depending on the model considered: inverse Compton emission via up-scattering of the synchrotron photons (synchrotron-self Compton model; Bloom & Marscher 1996), inverse Compton emission via upscattering of the external radiation photons (external Compton model, Ghisellini & Mandau 1996), emission from decays of neutral pions produced in proton-proton interactions (Nellen et al 1993;Bednarek & Protheroe 1997;Beall & Bednarek 1999;Neronov et al 2008;Neronov & Ribordy 2009;Barkov et al 2010), proton-photon interactions (Mannheim & Biermann 1992;Mannheim 1993;Bednariek & Protheroe 1999;Mücke & Protheroe 2001;Atoyan & Dermer 2001Neronov & Semikoz 2002) or proton synchrotron radiation (Mücke & Protheroe 2001;Aharonian 2000;Mücke et al 2003). The maximal attainable energy of γ-ray emission is limited either by the maximal energies of electrons or by the onset of γγ pair creation (Sikora et al 1987).…”

Section: Hadronic Models Of Blazar Activitymentioning

confidence: 99%

An exploration of hadronic interactions in blazars using IceCube

Tchernin

Aguilar

Neronov

et al. 2013

A&A

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Context. Hadronic models, involving matter (proton or nuclei) acceleration in blazar jets, imply high energy photon and neutrino emissions due to interactions of high-energy protons with matter and/or radiation in the source environment. Aims. This paper shows that the sensitivity of the IceCube neutrino telescope in its 40-string configuration (IC-40) is already at the level of constraining the parameter space of purely hadronic scenarios of activity of blazars. Methods. Assuming that the entire source power originates from hadronic interactions, and assuming that the model describe the data, we estimate the expected neutrino flux from blazars based on the observed γ-ray flux by Fermi, simultaneously with IC-40 observations. We consider two cases separately to keep the number of constrainable parameters at an acceptable level: proton-proton or proton-gamma interactions are dominant. Comparing the IC-40 sensitivity to the neutrino flux expected from some of the brightest blazars, we constrain model parameters characterizing the parent high-energy proton spectrum. Results. Using together the Fermi photon observations and the IC-40 neutrino sensitivities, we find that when pp interactions dominate, some constraints on the primary proton spectrum can be imposed. For instance, for the tightest constrained source 3C 454.3, the very high energy part of the spectra of blazars is constrained to be harder than E −2 with cut-off energies in the range of E cut ≥ 10 18 eV. When interactions of high-energy protons on soft photon fields dominate, we can find similarly tight constraints on the proton spectrum parameters if the soft photon field is in the UV range or at higher energy, e.g. if it originates from the "big blue bump" produced by the accretion disk. The tightest constraint is for 3C 273, with the cut-off energy constrained to be E cut 10 18 eV for any spectral index and different soft photon fields, including the radiation from the accretions disk, broad line region or the synchrotron radiation from the jet. Conclusions. We have adopted a simplified approach using the IC-40 sensitivity (about one half of the full detector) to constrain parameters of blazar hadronic models. Data of the full detector are already available and corresponding constraints should be about a factor of 3 better than what discussed here.

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Section: Hadronic Models Of Blazar Activitymentioning

confidence: 99%

An exploration of hadronic interactions in blazars using IceCube

Tchernin

Aguilar

Neronov

et al. 2013

A&A

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“…In leptonic models, γ-ray radiation from blazars is mostly explained by Compton scattering of low-energy synchrotron photons by the same relativistic electrons in the jets producing the synchrotron emission at lower frequencies (e.g., Bloom & Marscher, 1996); in hadronic models, the high-energy emission is dominated by relativistic protons (e.g., Böttcher, 2010). Besides the blazars, there are dozens of misaligned AGN detected by the Fermi (e.g., Abdo et al, 2010a;Ackermann et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Cui

Gabányi

et al. 2016

Astron Nachr

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Most of the γ-ray emitting active galactic nuclei (AGN) are blazars, although there is still a small fraction of non-blazar AGN in the Fermi/LAT catalog. Among these misaligned γ-ray-emitting AGN, a few can be classified as Compact Symmetric Objects (CSOs). In contrast to blazars in which γ-ray emission is generally thought to originate from highly beamed relativistic jets, the source of γ-ray emission in unbeamed CSOs remains an open question. The rarity of the γ-ray emitting CSOs is a mystery as well. Here we present the radio properties of the γ-ray CSO candidate 2234+282.

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“…The seed photons for ICs can originate from synchrotron photons (Maraschi et ⋆ Corresponding author. E-mail: ynzyg@ynu.edu.cn Bloom & Marscher 1996), accretion disk photons (Dermer et al 1992;Dermer & Schlickeiser 1993) and accretion disk photons re-scattered by the broad-line region clouds/interclouds medium (Sikora et al 1994;Blandford & Levinson 1995), or infrared radiation from a torus (Sikora et al 1994).…”

Section: Introductionmentioning

confidence: 99%

Modelling the multi-wavelength emission of flat-spectrum radio quasar 3C 279

Zheng

Yang

2016

Mon. Not. R. Astron. Soc.

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We employ a length-dependent conical jet model for the jet structure and emission properties of flat spectrum radio quasar 3C 279 in the steady state. In the model, ultrarelativistic leptons are injected at the base of jet and propagate along the jet structure, non-thermal photons are produced by both synchrotron emission and inverse Comtpon scattering off synchrotron photons and external soft photons at each segment of jet. We derive the total energy spectra contribution through integrating every segment. We apply the model to the quasi-simultaneous multi-wavelength observed data of two quiescent epoches. Using the observed radio data of source, we determine the length of jet L ∼ 100 pc, and magnetic field B 0 ∼ 0.1 − 1 G at the base of jet. Assuming a steady geometry of the jet structure and suitable physical parameters, we reproduce the multi-wavelength spectra during two quiescent observed epoches, respectively. Our results show that the initial γ-ray emission site takes place at ∼ 0.5 pc from black hole.

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An Analysis of the Synchrotron Self-Compton Model for the Multi--Wave Band Spectra of Blazars

Cited by 471 publications

References 0 publications

An exploration of hadronic interactions in blazars using IceCube

An exploration of hadronic interactions in blazars using IceCube

Radio properties of the γ ‐ray emitting CSO candidate 2234+282

Modelling the multi-wavelength emission of flat-spectrum radio quasar 3C 279

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