Hadronic jet models today

Sikora, Marek

doi:10.1017/s1743921310015644

Cited by 3 publications

(2 citation statements)

References 29 publications

(36 reference statements)

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“…As the cooling timescale is much longer than the escape timescale in the AGN jets (Böttcher et al 2013;Murase et al 2014;Gao et al 2017), the photohadronic interactions are very inefficient (Sikora et al 2009;Sikora 2011), and thus CRs readily escape from the the jets and host galaxy. It is usually difficult to estimate the baryon loading factor of AGNs using the radiation of AGNs (Protheroe & Szabo 1992;Berezhko 2008).…”

Section: Introductionmentioning

confidence: 99%

Constraining the baryon loading factor of AGN jets: implication from the gamma-ray emission of the Coma cluster

Shi,

Zhang,

Liu

et al. 2022

Preprint

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High-energy cosmic rays (CRs) can be accelerated in the relativistic jets of Active Galactic Nuclei (AGNs) powered by supermassive black holes. The baryon loading efficiency onto relativistic CR baryons from the accreting black holes is poorly constrained by observations so far. In this paper, we suggest that the γ-ray emission of galaxy clusters can be used to study the baryon loading factor of AGN jets, since CRs injected by AGN jets are completely confined in the galaxy clusters and sufficiently interact with intra-cluster medium via hadronic process, producing diffuse γ-rays. We study the propagation of CRs in the galaxy clusters and calculate the radial distribution of the gamma-rays in the galaxy cluster with different injection rates from AGNs. By comparison with the γ-ray flux and upper limits of the Coma cluster measured by F ermi-LAT and VERITAS, we find the upper limit of the average baryon loading factor (defined as the efficiency with which the gravitational energy is converted into relativistic particles) to be η p,grav < 0.1. The upper limit is much lower than that required to account for diffuse neutrino flux in the conventional blazar models.

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Section: Introductionmentioning

confidence: 99%

Constraining the baryon loading factor of AGN jets: implication from the gamma-ray emission of the Coma cluster

Shi,

Zhang,

Liu

et al. 2022

Preprint

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show abstract

“…[4]). An additional problem is that energy requirements are in general larger for hadronic than for leptonic scenarios [5]. Fig.…”

Section: Introductionmentioning

confidence: 99%

Signatures of relativistic protons in CTA blazar spectra

Zech,

Cerruti

2013

Preprint

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The Cherenkov Telescope Array (CTA) will provide very-high-energy (VHE; 30 GeV) γ-ray spectra of unprecedented resolution over a large energy range. It is likely that, at least for bright sources, spectral features will be revealed that cannot be distinguished with the current generation of Cherenkov telescopes. We are investigating the capability of the CTA to detect spectral signatures in TeV bright BL Lac objects that could reveal the emission from a population of relativistic protons in those sources. Such a detection would be crucial for the long-standing question of the origin of extragalactic cosmic rays. As a first step, the expected VHE emission from hadronic scenarios is compared to the spectral features that might arise in the more commonly assumed leptonic scenarios for a given source. We also evaluate the impact of different array configurations on the detectability of such features.

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EVIDENCE FOR SECONDARY EMISSION AS THE ORIGIN OF HARD SPECTRA IN TeV BLAZARS

Zheng

Kang

2013

ApJ

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We develop a model for the possible origin of hard, very high energy (VHE) spectra from a distant blazar. In the model, both the primary photons produced in the source and secondary photons produced outside it contribute to the observed high-energy γ -ray emission. That is, the primary photons are produced through the synchrotron self-Compton process, and the secondary photons are produced through high-energy proton interactions with background photons along the line of sight. We apply the model to a characteristic case of VHE γ -ray emission in the distant blazar 1ES 1101-232. Assuming suitable electron and proton spectra, we obtain excellent fits to the observed spectra of this blazar. This indicated that the surprisingly low attenuation of the high-energy γ -rays, especially the shape of the VHE γ -ray tail of the observed spectra, can be explained by secondary γ -rays produced in interactions of cosmic-ray protons with background photons in intergalactic space.

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Hadronic jet models today

Cited by 3 publications

References 29 publications

Constraining the baryon loading factor of AGN jets: implication from the gamma-ray emission of the Coma cluster

Constraining the baryon loading factor of AGN jets: implication from the gamma-ray emission of the Coma cluster

Signatures of relativistic protons in CTA blazar spectra

EVIDENCE FOR SECONDARY EMISSION AS THE ORIGIN OF HARD SPECTRA IN TeV BLAZARS

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