A Hadronic Synchrotron Mirror Model for the “Orphan” TeV Flare in 1ES 1959+650

Böttcher, M.

doi:10.1086/427430

Cited by 63 publications

(64 citation statements)

References 33 publications

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“…However, in the hadronic models, no necessary correlations between the spectral components are expected. Correlated variations across SEDs observed in some blazars seem to be consistent with the leptonic models, but the so-called orphan flares observed in some TeV blazars prefer the hadronic scenarios (e.g., Bonning et al 2012;Böttcher 2005). A long-term optical variability monitoring program for blazars has been performed at Yunnan Observatories (e.g., Bai et al 1998).…”

Section: Introductionmentioning

confidence: 82%

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

Liao

Bai

Liu

et al. 2014

ApJ

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S5 0716+714 is a typical BL Lacertae object. In this paper we present the analysis and results of long-term simultaneous observations in the radio, near-infrared, optical, X-ray, and γ -ray bands, together with our own photometric observations for this source. The light curves show that the variability amplitudes in γ -ray and optical bands are larger than those in the hard X-ray and radio bands and that the spectral energy distribution (SED) peaks move to shorter wavelengths when the source becomes brighter, which is similar to other blazars, i.e., more variable at wavelengths shorter than the SED peak frequencies. Analysis shows that the characteristic variability timescales in the 14.5 GHz, the optical, the X-ray, and the γ -ray bands are comparable to each other. The variations of the hard X-ray and 14.5 GHz emissions are correlated with zero lag, and so are the V band and γ -ray variations, which are consistent with the leptonic models. Coincidences of γ -ray and optical flares with a dramatic change of the optical polarization are detected. Hadronic models do not have the same natural explanation for these observations as the leptonic models. A strong optical flare correlating a γ -ray flare whose peak flux is lower than the average flux is detected. The leptonic model can explain this variability phenomenon through simultaneous SED modeling. Different leptonic models are distinguished by average SED modeling. The synchrotron plus synchrotron selfCompton (SSC) model is ruled out because of the extreme input parameters. Scattering of external seed photons, such as the hot-dust or broad-line region emission, and the SSC process are probably both needed to explain the γ -ray emission of S5 0716+714.

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Section: Introductionmentioning

confidence: 82%

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

Liao

Bai

Liu

et al. 2014

ApJ

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“…model [7,26]. Similarly, the recent spine-sheath model [27] predicts only 0.04 additional neutrino events on the days of the brightest flares, where the gamma ray flux levels reach 10-15 times that of the low state [11].…”

Section: Pos(icrc2017)969mentioning

confidence: 88%

“…A simple Synchrotron Self Compton (SSC) one [5] was found to underpredict the observed radio and optical fluxes. Alternatively, hadronic models, such as the "mirror model" [7] were also developed for this event and predict a correlated neutrino flux.…”

Section: Introductionmentioning

confidence: 99%

IceCube Search for Neutrinos from 1ES 1959+650: Completing the Picture

Kintscher¹,

Krings²,

Dorner³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The IceCube neutrino observatory is a 1 km 3 detector deployed in the ice at the South Pole. While it has observed an astrophysical flux of neutrinos, individual sources have yet to be identified and the high-peaked BL Lac object 1ES 1959+650 is an intriguing candidate. It exhibited an "orphan flare" in 2002: a TeV gamma ray flare without a simultaneous X-ray flare, behavior that is hard to accommodate in leptonic synchrotron self-compton models. This suggests that it is a potential site of hadronic acceleration and thus a prime source candidate for neutrinos. A recently observed increase in gamma ray activity from 1ES 1959+650 between May and July of 2016 has provided a new opportunity, prompting a dedicated search in IceCube data for neutrinos correlated with the flaring states during this period. We present results based on two model-independent approaches which look only for an excess of neutrinos from the source, as well as a more targeted search for a direct time correlation between neutrino events observed by IceCube and gamma ray emission observed with the FACT and MAGIC telescopes.

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“…Here we further assume that the ratio of photon densities at different energies in the flaring and non-flaring states are the same. This scenario neither needs any intervening foreign object nor any special jet cloud geometry [29] to produce the high energy photons.…”

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 Hadronic Synchrotron Mirror Model for the “Orphan” TeV Flare in 1ES 1959+650

Cited by 63 publications

References 33 publications

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

MULTIWAVELENGTH VARIABILITY PROPERTIES OFFERMIBLAZAR S5 0716+714

IceCube Search for Neutrinos from 1ES 1959+650: Completing the Picture

Hadronic origin of the TeV flare of M87 in April 2010

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