A two-component model for the high-energy variability of blazars

Reynoso, Matías M.; Romero, Gustavo E.; Medina, M. C.

doi:10.1051/0004-6361/201219873

Cited by 22 publications

(24 citation statements)

References 36 publications

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“…These fast variability of blazars indicate substantial sub-structure in their jets, which may be due to turbulence or as a result of magnetic reconnection Giannios et al 2009;Reynoso et al 2012). Rapid variability also implies significant beaming effect of TeV HSP BL Lacs including PKS 2155-304.…”

Section: The Spine/layer Jetmentioning

confidence: 98%

The Hard X-Ray Emission of the Blazar PKS 2155–304

Gaur¹,

Chen²,

Misra³

et al. 2017

ApJ

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The synchrotron peak of the X-ray bright High Energy Peaked Blazar (HBL) PKS 2155−304 occurs in the UV-EUV region and hence its X-ray emission (0.6-10 keV) lies mostly in the falling part of the synchrotron hump. We aim to study the X-ray emission of PKS 2155−304 during different intensity states in 2009−2014 using XMM−Newton satellite. We studied the spectral curvature of all of the observations to provide crucial information on the energy distribution of the non-thermal particles. Most of the observations show curvature or deviation from a single power-law and can be well modeled by a log parabola model. In some of the observations, we find spectral flattening after 6 keV. In order to find the possible origin of the X-ray excess, we built the Multi-band Spectral Energy distribution (SED). We find that the X-ray excess in PKS 2155-304 is difficult to fit in the one zone model but, could be easily reconciled in the spine/layer jet structure. The hard X-ray excess can be explained by the inverse Comptonization of the synchrotron photons (from the layer) by the spine electrons.

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Section: The Spine/layer Jetmentioning

confidence: 98%

The Hard X-Ray Emission of the Blazar PKS 2155–304

Gaur¹,

Chen²,

Misra³

et al. 2017

ApJ

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“…3. For a self consistent treatment, in principle, we should use the photon density n γ, f in the hidden internal jet and solve the coupled transport equations for leptons and photons along the jet axis by taking into account their respective cooling mechanisms as well as the injection spectrum of the primary particles [34]. To avoid this complication we assume the scaling behavior of the photon densities in different background energies as follows:…”

Section: Photohadronic Modelmentioning

confidence: 99%

Multi-TeV flaring from blazars: Markarian 421 as a case study

2016

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The TeV blazar Markarian 421 underwent multiTeV flaring during April 2004 and simultaneously observations in the X-ray and TeV energies were made. It was observed that the TeV outbursts had no counterparts in the lower energy range. One implication of this is that it might be an orphan flare. We show that Fermi-accelerated protons of energy ≤168 TeV can interact with the low energy tail of the background synchrotron self-Compton photons in the inner region of the blazar to produce the multi-TeV flare and our results fit very well with the observed spectrum. Based on our study, we predict that the blazars with a deep valley in between the end of the synchrotron spectrum and the beginning of the SSC spectrum are possible candidates for orphan flaring. Future possible candidates for this scenario are the HBLs Mrk 501 and PG 1553 + 113 objects.

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“…(12). A better approach is to solve self consistently the coupled transport equations for leptons and photons along the jet by taking into account their respective cooling mechanisms as well as the injection spectrum of the primary particles [18]. To avoid this complication we assume the scaling behavior of photon number densities in different regions as discussed above and then use the one-zone leptonic model fit to the SED of M87 for the calculation of the flaring events.…”

Section: The Flaring Modelmentioning

confidence: 99%

“…The lepto-hadronic model [17] fits to the low energy γ -ray spectrum by Fermi/LAT and HESS low state but not the flaring state. However, this model has been extended by Reynoso et al [18] to study the production of very high energy γ -rays in blazars by introducing a two-components jet. The spine-sheath model by Tavecchio and Ghiselline [19] has difficulties to achieve a harder spectrum in the VHE range due to strong absorption of the TeV photons from interactions with the optical-infra red (IR) photons from the spine.…”

Section: Introductionmentioning

confidence: 99%

Hadronic origin of the TeV flare of M87 in April 2010

Sahu

Palacios

2015

Eur. Phys. J. C

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M87 is a giant radio galaxy with FR-I morphology. It underwent three episodes of TeV flaring in recent years with the strongest one in April 2010 which was jointly monitored by MAGIC, VERITAS and H.E.S.S. We explain its spectral energy distribution in the energy range 0.3-5 TeV by assuming that the flaring occurs in the innermost region of the jet. In this region the low energy SSC photons serve as the target for the Fermi-accelerated high energy protons of energy ≤30 TeV to form a delta resonance. The TeV photons are produced from the subsequent decay of the delta resonance to neutral pions. In this scenario the observed TeV flux of April 2010 flare is fitted very well.

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A two-component model for the high-energy variability of blazars

Cited by 22 publications

References 36 publications

The Hard X-Ray Emission of the Blazar PKS 2155–304

The Hard X-Ray Emission of the Blazar PKS 2155–304

Multi-TeV flaring from blazars: Markarian 421 as a case study

Hadronic origin of the TeV flare of M87 in April 2010

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