Photohadronic scenario in interpreting the February–March 2014 flare of 1ES 1011+496

Sahu, Sarira; León, Alberto Rosales de; Miranda, Luis Salvador

doi:10.1140/epjc/s10052-017-5335-2

Cited by 8 publications

(8 citation statements)

References 44 publications

(56 reference statements)

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“…The source is also listed in the second catalog of hard Femi-LAT sources. A photohadronic scenario to explain the high-energy SED is employed in Sahu et al (2017). The flux value of the low-and high-energy peak are comparable.…”

Section: Resultsmentioning

confidence: 99%

Ultrahigh-energy Cosmic-Ray Interactions as the Origin of Very High-energy γ-Rays from BL Lacertae Objects

Das

Gupta

Razzaque³

2020

ApJ

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We explain the observed multiwavelength photon spectrum of a number of BL Lac objects detected at very high energy (VHE, E 30 GeV), using a lepto-hadronic emission model. The one-zone leptonic emission is employed to fit the synchrotron peak. Subsequently, the SSC spectrum is calculated, such that it extends up to the highest energy possible for the jet parameters considered. The data points beyond this energy, and also in the entire VHE range are well explained using a hadronic emission model. The ultrahigh-energy cosmic rays (UHECRs, E 0.1 EeV) escaping from the source interact with the extragalactic background light (EBL) during propagation over cosmological distances to initiate electromagnetic cascade down to ∼ 1 GeV energies. The resulting photon spectrum peaks at ∼ 1 TeV energies. We consider a random turbulent extragalactic magnetic field (EGMF) with a Kolmogorov power spectrum to find the survival rate of UHECRs within 0.1 degrees of the direction of propagation in which the observer is situated. We restrict ourselves to an RMS value of EGMF, B rms ∼ 10 −5 nG, for a significant contribution to the photon spectral energy distribution (SED) from UHECR interactions. We found that UHECR interactions on the EBL and secondary cascade emission can fit gamma-ray data from the BL Lacs we considered at the highest energies. The required luminosity in UHECRs and corresponding jet power are below the Eddington luminosities of the super-massive black holes in these BL Lacs.

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Section: Resultsmentioning

confidence: 99%

Ultrahigh-energy Cosmic-Ray Interactions as the Origin of Very High-energy γ-Rays from BL Lacertae Objects

Das

Gupta

Razzaque³

2020

ApJ

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“…The photohadronic model of Sahu et al [15,16,21,22] can explain the flaring events from HBLs very well and it relies on the standard interpretation of the leptonic model discussed above to explain both low and high energy peaks by synchrotron and SSC photons respectively as in the case of any other AGN.…”

Section: The Modelmentioning

confidence: 99%

The VHE SED modelling of Markarian 501 in 2009

Sahu

Fortín

Martínez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The high energy blazar, Markarian 501 was observed as a part of multi-instrument and multiwavelength campaign spanning the whole electromagnetic spectrum for 4.5 months during March 15 to August 1, 2009. On May 1, Whipple 10m telescope observed a very strong γ-ray flare in a time interval of about 0.5 h. Apart from this flare, high state and low state emissions were also observed by Whipple, VERITAS and MAGIC telescopes. Using the photohadronic model and accounting for the absorption of the extragalactic background light (EBL) to these very high energy γ-rays, excellent fits are obtained for the observed spectra. We have shown that the intrinsic spectrum for low state emission is flat, however, for high and very high states this is a power-law with slowly increasing exponent.

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“…The photohadronic model [19,20,30,38] In the compact inner jet region, the Fermi accelerated high energy protons interact with the background photons with a comoving density n γ,f to produce the ∆-resonance and its subsequent decay to neutral and charged pions will give VHE γ-rays and neutrinos respectively. In the flaring region we assume n γ,f is much higher than the rest of the blob n γ (non-flaring) i.e.…”

Section: Photohadronic Modelmentioning

confidence: 99%

The nature of the intrinsic spectra from the VHE emission of H 2356-309 and 1ES 1101-232

2018

Self Cite

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were analyzed to derive strong upper limits on the EBL, which were found to be consistent with the lower limits from the integrated light of resolved galaxies. Here we have used the photohadronic model corroborated by two template EBL models to fit the observed VHE gamma-ray data from these two HBLs and to predict their intrinsic spectra. We obtain very good fit to the VHE spectra of these two HBLs. However, the predicted intrinsic spectra are different for each EBL model. For the HBL H 2356-309, we obtain a flat intrinsic spectrum and for 1ES 1101-232 the spectrum is mildly harder than 2 but much softer than 1.5.

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Photohadronic scenario in interpreting the February–March 2014 flare of 1ES 1011+496

Cited by 8 publications

References 44 publications

Ultrahigh-energy Cosmic-Ray Interactions as the Origin of Very High-energy γ-Rays from BL Lacertae Objects

Ultrahigh-energy Cosmic-Ray Interactions as the Origin of Very High-energy γ-Rays from BL Lacertae Objects

The VHE SED modelling of Markarian 501 in 2009

The nature of the intrinsic spectra from the VHE emission of H 2356-309 and 1ES 1101-232

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