EBL effect on the observation of multi-TeV flaring of 2009 from Markarian 501

Sahu, Sarira; Yáñez, Marco Vladimir Lemus; Miranda, Luis Salvador; León, Alberto Rosales de; Gupta, Virendra K.

doi:10.1140/epjc/s10052-016-4592-9

Cited by 9 publications

(9 citation statements)

References 37 publications

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“…This difference in intrinsic spectra attributes to the change in the spectral index of the seed photon in the SSC tail region of the jet in different epochs of flaring. The same photohadronic models were earlier employed to explain the multi-TeV emission from other HBLs [57,59]. We suggest that the same flaring mechanism may be acting in all HBLs.…”

Section: Discussionsupporting

confidence: 65%

The origin of multi-TeV flares from the nearest blazar Markarian 421

et al. 2018

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Markarian 421 is a high-peaked BL Lac object and it has undergone many strong outbursts since its discovery as a TeV source in 1992. Markarian 421 has been studied intensively and was observed by various Cherenkov telescope arrays ever since. The outbursts of April 2004 observed by the Whipple telescope and of February 2010 by the HESS telescopes are explained well in this work by using the photohadronic model. To account for the attenuation of these highenergy gamma-rays by the extragalactic background light (EBL), we use template EBL models. The intrinsic spectrum of each epoch is different even though the high-energy protons have almost the same spectral index. We observe that this difference in intrinsic spectra is due to the change in the spectral index of the low-energy tail of the synchrotron self Compton (SSC) photons during different epochs of flaring. Our results show that the contemporaneous multiwavelength observations, particularly in the low-energy tail region of the SSC emission of the source, are important in explaining the flaring phenomenon.

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Section: Discussionsupporting

confidence: 65%

The origin of multi-TeV flares from the nearest blazar Markarian 421

et al. 2018

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“…So the unknown internal photon density is expressed in terms of the known photon density calculated from the observed/fitted SED in the SSC region, which is again related to the observed flux in the same region. This model explains very nicely the observed TeV flux from the orphan flares of 1ES 1959+650, Mrk 421 as well as the multi-TeV flaring from M87 and Mrk 501 [29][30][31]39]. In the observer frame, the π 0 -decay photon energy E γ and the background SSC photon energy γ are related through…”

Section: Photohadronic Modelsupporting

confidence: 52%

“…For far-off sources the EBL plays the dominant role, which shows that E γ,c is much higher than the highest energy γ -ray observed during the VHE flaring event. Recently we have shown [39] that for nearby objects the EBL effect is also important and there is no need of an exponential cut-off. Including the EBL effect in the photohadronic scenario [30] the observed multi-TeV flux is expressed as…”

Section: Photohadronic Modelmentioning

confidence: 99%

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

2017

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The extraordinary multi-TeV flare from 1ES 1011+496 during February-March 2014 was observed by the MAGIC telescopes for 17 nights and the average spectrum of the whole period has a non-trivial shape. We have used the photohadronic model and a template extragalactic background light model to explain the average spectrum which fits the flare data well. The spectral index α is the only free parameter in our model. We have also shown that the non-trivial nature of the spectrum is due to the change in the behavior of the optical depth above ∼ 600 GeV γ -ray energy accompanied with the high SSC flux. This corresponds to an almost flat intrinsic flux for the multi-TeV γ -rays. Our model prediction can constrain the SSC flux of the leptonic models in the quiescent state.

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“…The very strong VHE flare data of May 1st observed by Whipple telescope and the long outburst observed by HEGRA telescopes in 1997 were modeled using the photohadronic model of ref. [39]. The model of Dominguez et al [46] is used to correct for the EBL effect on the observed data.…”

Section: A Markarian 421mentioning

confidence: 99%

Multi-TeV flaring in nearby high-energy blazars: A photohadronic scenario

Sahu

2019

Rev. Mex. Fís.

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Blazars are a subclass of AGN and flaring in multi-TeV gamma-ray seems to be the major activity in high energy blazars a subgrup of blazars. Flaring is also unpredictable and switches between quiescent and active states involving different time scales and fluxes. While in some high energy blazars a strong temporal correlation between X-ray and multi-TeV gamma-ray has been observed, outbursts in some other have no low energy counterparts and explanation of such extreme activity needs to be addressed through different mechanisms as it is not understood well. The extragalactic background light (EBL) plays an important role in the observation of these high energy gamma-rays as it attenuates through pair production of electron-positron and also changes the spectral shape of the high energy photons. In the context of the photohadronic model and taking EBL correction into account, flaring can be explained very well. In a series of papers we have developed this model to explain multi-TeV flaring events form many blazars. Here in this review, the photohadronic model is discussed and applied to explain the multi-TeV flaring from nearby high energy blazars: Markarian 421, Markarian 501 and 1ES1959+650. * sarira@nucleares.unam.mx 1 arXiv:1907.01174v1 [astro-ph.HE]

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EBL effect on the observation of multi-TeV flaring of 2009 from Markarian 501

Cited by 9 publications

References 37 publications

The origin of multi-TeV flares from the nearest blazar Markarian 421

The origin of multi-TeV flares from the nearest blazar Markarian 421

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

Multi-TeV flaring in nearby high-energy blazars: A photohadronic scenario

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