Multiwavelength Observations of Strong Flares from the TeV Blazar 1ES 1959+650

Krawczynski, H.; Hughes, Shaun M. G.; Horan, D.; Aharonian, F.; Aller, M. F.; Aller, H. D.; Boltwood, P.; Buckley, J. H.; Coppi, P.; Fossati, G.; Götting, N.; Holder, J.; Horns, D.; Kurtanidze, O. M.; Marscher, A. P.; Nikolashvili, M. G.; Remillard, Ron; Sadun, A. C.; Schroder, Matthias

doi:10.1086/380393

Cited by 380 publications

(474 citation statements)

References 52 publications

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“…This prediction is in striking contrast to the recent observation of Krawczynski et al (2004) of an ''orphan'' TeV flare in the Whipple light curve of the TeV blazar 1ES 1959+650 during a multiwavelength campaign in the late spring and summer of 2002. The object displayed first a quasi-simultaneous TeV and X-ray (Rossi X-Ray Timing Explorer [RXTE]) flare, and then a well-sampled, smooth decline of the X-ray flux over the following $1 month.…”

Section: Introductioncontrasting

confidence: 99%

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

Böttcher

2005

ApJ

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Very high energy -ray flares of TeV blazars are generally accompanied by simultaneous flaring activity in X-rays. The recent observations by the Whipple collaboration of an ''orphan'' TeV flare of 1ES 1959+650 (without a simultaneous X-ray flare) are very difficult to reconcile with the standard leptonic synchrotron self-Compton model, which is routinely very successfully employed to explain the spectral energy distribution and spectral variability of TeV blazars. In this paper an alternative scenario is suggested in which the orphan TeV flare may originate from relativistic protons, interacting with an external photon field supplied by electron synchrotron radiation reflected off a dilute reflector. While the external photons will be virtually ''invisible'' to the comoving ultrarelativistic electrons in the jet because of Klein-Nishina effects, their Doppler-boosted energy is high enough to excite a Á-resonance from relativistic protons with Lorentz factors of p $ 10 3 10 4 . This model is capable of explaining the orphan TeV flare of 1ES 1959+650 with plausible parameters, thus constraining the number and characteristic energy of relativistic protons in the jet of this blazar.

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Section: Introductioncontrasting

confidence: 99%

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

Böttcher

2005

ApJ

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“…This was reported at least two times (e.g. Krawczynski et al 2004;Blazejowski et al 2005) and is know in the literature as an orphan flare phenomenon.…”

Section: The Observations Of Mrk 421 Made In March 2001mentioning

confidence: 80%

On the correlation between the X-ray and gamma-ray emission in TeV blazars

Walczewska¹

2010

A&A

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Aims. The observations of TeV blazars published recently show an unexpected quadratic or even cubic correlation between the X-ray and gamma-ray emission. A standard model of the synchrotron self-Compton emission of a compact source inside a jet is not able to explain such a correlation. Therefore, we propose an alternative scenario where the emission of at least two independent compact components is observed at the same time. Methods. We compare two different models. The first model assumes the injection of relativistic particles into a downstream region of a shock wave inside a jet that creates the emitting source. The model precisely describes the evolution of the particle energy spectrum inside the source and takes into account a light-crossing time effect for the produced radiation. The second model assumes an intrinsically constant emission of a homogeneous source that travels inside the jet along a curved trajectory, where the activity is produced simply by different values of the source's Doppler factor. To verify the two models we use recently published observations of Mrk 421. Results. Our simulations show that simultaneous radiation of at least two independent sources, where the first source dominates the emission in the X-ray range and the second source radiates strongly in the gamma-ray range, can explain the observed correlations. However, the injection model provides inadequate results because it gives different values for the correlation of the rise and decay of a flare. This problem is negligible in the scenario that uses the Doppler boosting effect. Therefore, this approach yields much better results.

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“…Krawczynski et al 2004;Gliozzi et al 2006;Zhang et al 2006), e.g. due to shock acceleration of electrons in a jet producing both higher energy synchrotron seed photons and higher energy (inverse) Compton scattering.…”

Section: Correlations Between Photon Index and Luminositymentioning

confidence: 99%

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

Connolly

McHardy

Skipper

et al. 2016

Mon. Not. R. Astron. Soc.

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We present X-ray spectral variability of 24 local active galactic nuclei (AGN) from the Palomar sample of nearby galaxies, as observed mainly by Swift. From hardness ratio measurements, we find that 18 AGN with low accretion rates show hardening with increasing count rate, converse to the softer-when-brighter behaviour normally observed in AGN with higher accretion rates. Two AGN show softening with increasing count rate, two show more complex behaviour, and two do not show any simple relationship.Sufficient data were available for the spectra of 13 AGN to be summed in fluxbins. In 9 of these sources, correlated luminosity-dependent changes in the photon index (Γ) of a power-law component are found to be the main cause of hardness variability. For 6 objects, with a low accretion rate as a fraction of the Eddington rate (ṁ Edd ), Γ is anticorrelated withṁ Edd , i.e. 'harder-when-brighter' behaviour is observed. The 3 higher-ṁ Edd -rate objects show a positive correlation between Γ anḋ m Edd . This transition from harder-when-brighter at lowṁ Edd to softer-when-brighter at highṁ Edd can be explained by a change in the dominant source of seed-photons for X-ray emission from cyclo-synchrotron emission from the Comptonising corona itself to thermal seed-photons from the accretion disc. This transition is also seen in the 'hard state' of black hole X-ray binaries (BHXRBs). The results support the idea that LINERs are analogues of BHXRBs in the hard state and that Seyferts are analogues of BHXRBs in either the high-accretion-rate end of the hard state or in the hard-intermediate state.

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Multiwavelength Observations of Strong Flares from the TeV Blazar 1ES 1959+650

Cited by 380 publications

References 52 publications

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

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

On the correlation between the X-ray and gamma-ray emission in TeV blazars

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

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