A jet model for the gamma-ray emitting blazar 3C 279

Maraschi, L.; Ghisellini, G.; Celotti, A.

doi:10.1086/186531

Cited by 1,063 publications

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“…Even though their output in the γ-ray domain often dominates the bolometric luminosity of these sources, the location of the region responsible for this intense γ-ray radiation remains unclear. The potential connection of this region to the vicinities of the central supermassive black hole (SMBH) is complicated by the fact that the multi-GeV gamma rays may be absorbed in the dense optical and UV photon fields (Jelley 1966), originating from the broad line region (BLR; Liu & Bai 2006;Poutanen & Stern 2010), jet, or accretion flow (Dermer et al 1992;Maraschi et al 1992;Bednarek 1993). A solution to this problem is found in the assumption that the gamma ray emission site is located at parsec-scale distances from the SMBH where the photon fields are less intense and the γ-ray emission can escape the source (Abdo et al 2010;Tavecchio et al 2011;Pacciani et al 2012;Ghisellini et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Vovk

Babić

2015

A&A

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Context. The variability time scales of the blazar γ-ray emission contain the imprints of the sizes of their emission zones and are generally expected to be larger than the light-crossing times of these zones. In several cases the time scales were found to be as short ∼10 min, suggesting that the emission zone sizes are comparable with the sizes of the central supermassive black holes. Previously, these measurements also led to the suggestion of a possible connection between the observed minimal variability time scales and the masses of the corresponding black holes. This connection can be used to determine the location of the γ-ray emission site, which currently remains uncertain. Aims. The study aims to investigate the suggested "minimum time scale -black hole mass" relation using the blazars, detected in the TeV band. Methods. To obtain the tightest constraints on the variability time scales this work uses a compilation of observations by the Cherenkov telescopes HESS, MAGIC, and VERITAS. These measurements are compared to the blazar central black hole masses found in the literature.Results. The majority of the studied blazars show the variability time scales which are at least comparable to the period of rotation along the last stable orbit of the central black hole -and in some cases as short as its light-crossing time. For several sources the observed variability time scales are found to be smaller than the black hole light-crossing time. This suggests that the detected γ-ray variability originates, most probably, from the turbulence in the jet, sufficiently far from the central black hole.

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Section: Introductionmentioning

confidence: 99%

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Vovk

Babić

2015

A&A

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“…In leptonic emission models (for review see Böttcher 2007) synchrotron radiation from highly relativistic electrons generates the low-energy component whereas the high-energy component results from Compton interactions of the same relativistic electron population. A prime candidate for the source photons being Compton upscattered are the selfproduced synchrotron photons, which defines the synchrotron self-Compton (SSC) process (e.g., Maraschi et al 1992;Bloom & Marscher 1996). Because of the short radiative synchrotron and SSC cooling time scales it is necessary to calculate selfconsistently the time evolution of the energy spectrum of the radiating relativistic electrons when modeling the spectral energy distribution (SED) from these objects.…”

Section: Introductionmentioning

confidence: 99%

Combined synchrotron and nonlinear synchrotron-self-Compton cooling of relativistic electrons

Schlickeiser¹,

Böttcher

Menzler³

2010

A&A

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The broadband SEDs of blazars exhibit two broad spectral components, which in leptonic emission models are attributed to synchrotron radiation and SSC radiation of relativistic electrons. During high state phases, the high-frequency SSC component often dominates the low-frequency synchrotron component, implying that the inverse Compton SSC losses of electrons are at least equal to or greater than the synchrotron losses of electrons. The linear synchrotron cooling, usually included in radiation models of blazars, then has to be supplemented by the SSC cooling. Here, we present an analytical solution to the kinetic equation of relativistic electrons subject to the combined synchrotron and nonlinear synchrotron self-Compton cooling for monoenergetic injection. We calculate the time-dependent fluxes and time-integrated fluences resulting from monoenergetic electrons cooling via synchrotron and SSC, and suggest this as a model for the broadband SED of Compton-dominated blazars.

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“…Spectral energy density measurements constrain both the models of the jets and of the infrared photon density in the intervening intergalactic medium. The possibility of absorption of g-rays by IR radiation has been predicted for some time (Nikishov 1962;Gould & Schrèder 1967;Stecker, De Jager, & Salamon 1992), and implications of recent observations have been discussed (see, e.g., Biller et al 1998; Stanev100 keV attributed to synchrotron radiation from electrons and a higher one with energies sometimes extending to the TeV range, usually attributed to inverse Compton (IC) scattering (see, e.g., Maraschi, Ghisellini, & Celotti 1992;Marscher & Travis 1996). There are also competing models (Mannheim & Biermann 1992;Mannheim 1993Mannheim , 1998) that assume that the higher energy component arises from protons, either by proton-induced synchrotron cascades or by decays and/or interactions of secondary particles such as neutral pions and neutrons, or synchrotron radiation from proton beams (Mücke & Protheroe 2001;Aharonian 2000).…”

Section: Introductionmentioning

confidence: 99%

Cutoff in the T[CLC]e[/CLC]V Energy Spectrum of Markarian 421 during Strong Flares in 2001

Krennrich

Badran

Bond

et al. 2001

The Astrophysical Journal

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Exceptionally strong and long-lasting flaring activity of the blazar Mrk 421 occurred between 2001 January and March. Based on the excellent signal-to-noise ratio of the data, we derive the energy spectrum between 260 GeV and 17 TeV with unprecedented statistical precision. The spectrum is not well described by a simple power law even with a curvature term. Instead, the data can be described by a power law with exponential cutoff: with TeV. Mrk 421 is the second g-ray blazar thatunambiguously exhibits an absorption-like feature in its spectral energy distribution at 3-6 TeV. Subject headings: BL Lacertae objects: individual (Markarian 421) -gamma rays: observationsSince the discovery of TeV g-rays from BL Lac objects Mrk 421 (Punch et al. 1992) and Mrk 501 (Quinn et al. 1996), detailed very high energy observations of these nearby blazars (z p , ) have been made. Measurements of flux var-0.031 z p 0.034 iation with time, particularly simultaneous measurements at several wavelengths, constrain models of particle acceleration and g-ray production in the jets. Spectral energy density measurements constrain both the models of the jets and of the infrared photon density in the intervening intergalactic medium. The possibility of absorption of g-rays by IR radiation has been predicted for some time (Nikishov 1962;Gould & Schrèder 1967;Stecker, De Jager, & Salamon 1992), and implications of recent observations have been discussed (see, e.g., Biller et al. 1998;Stanev & Franceschini 1998;Vassiliev 1999).The general picture that has emerged for the spectral energy density of emitted radiation from BL Lac objects has two components: a lower one with energies extended up to about

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A jet model for the gamma-ray emitting blazar 3C 279

Cited by 1,063 publications

References 0 publications

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Combined synchrotron and nonlinear synchrotron-self-Compton cooling of relativistic electrons

Cutoff in the T[CLC]e[/CLC]V Energy Spectrum of Markarian 421 during Strong Flares in 2001

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