Radiation from relativistic beams interacting with interstellar gas

Rose, William K.; Beall, J. H.; Guillory, J.; Kainer, S.

doi:10.1086/165042

Cited by 19 publications

(14 citation statements)

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“…A more detailed discussion of the considerations leading to these rate equations can be found in Scott et al (1981), Rose et al (1984Rose et al ( , 1987, Beall et al (1987), and Beall (1990). The results of these estimates have been substantially conÐrmed by a PIC code simulation Rose et al 1998) in parameter ranges in which PIC code simulations are computationally practicable. The introduction of a weak, longitudinal magnetic Ðeld along the beam axis stabilizes the beam against a Ðlamentation instability and increases its propagation length somewhat.…”

Section: Propagation Of Relativistic Electron-proton Beams Through Inmentioning

confidence: 99%

“…Burbidge (1956), Felten (1968, Rose et al (1987), and Beall et al (1987) have suggested that hadronic interactions between the jet and the ambient medium in an AGN could produce high-energy c-rays. Rose et al (1984Rose et al ( , 1987 Ðrst calculated in detail the mechanisms of energy loss for a relativistic, low-density beam of electrons, electrons and positrons, or electrons and protons as it interacts with clouds in the BLR and NLR of AGNs. This work has been ampliÐed by a number of authors, including Beall (1990) and Dar & Laor (1997).…”

Section: Hadronic Jets In Active Galaxiesmentioning

confidence: 99%

“…Such magnetic Ðeld geometries in the inner core radio jets are inferred from jet polarization studies as Begelman et al (1984) and Saikia & Salter (1988) note. and Rose et al (1998) have conducted "" benchmark ÏÏ studies of the propagation model discussed below using a fully relativistic, two-dimensional particle-incell (PIC) code with a co-linear magnetic Ðeld but in a parameter range that is practicable for the PIC code algorithms. The propagation lengths derived with the PIC code are in substantial agreement with the calculations presented here.…”

Section: Propagation Of Relativistic Electron-proton Beams Through Inmentioning

confidence: 99%

“…Collisionless processes principally driven by the twostream instability (Scott et al 1980 ;Rose et al 1984Rose et al , 1987 can be the dominant energy-loss mechanism for such jets in parameter ranges associated with the BLR and narrow-line region (NLR) (Beall 1990). The computations by Dar & Laor do not take into account these collisionless energy losses as the jet propagates through the dense, hot medium of the cloud.…”

Section: Introductionmentioning

confidence: 99%

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On the Hadronic Beam Model for Gamma‐Ray Production in Blazars

Beall

Bednarek

1999

ApJ

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We consider a model for c-ray production in blazars in which a relativistic, highly collimated electronproton beam interacts with a dense, compact cloud as the jet propagates through the broad-and perhaps narrow-line regions of active galactic nuclei. During the propagation of the beam through the cloud, the process of excitation of plasma waves becomes an important energy-loss mechanism, especially for mildly relativistic proton beams. We compute the expected spectra of c-rays from the decay of neutral pions produced in hadronic collisions of the beam with the cloud, taking into account collisionless losses of the electron-proton beam. This model may explain the X-ray and TeV c-ray (both low and high emission states) of Mrk 421 as a result of synchrotron emission of secondary pairs from the decay of charged pions and c-ray emission from the decay of neutral pions for the plausible cloud parameters. However, clouds cannot be too hot and too dense. Otherwise, the TeV c-rays can be attenuated by the bremsstrahlung radiation in the cloud and the secondary pairs are not able to efficiently produce synchrotron Ñares because of the dominant role of inverse Compton scattering. The nonvariable c-ray emission observed from Mrk 421 in the EGRET energy range cannot be described by the c-rays from decay of neutral pions provided that the spectrum of protons in the beam is well described by a simple power law. These c-rays might only be produced by secondary pairs scattering the soft nonvariable X-rays, which might originate in the inner part of the accretion disk.

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Section: Propagation Of Relativistic Electron-proton Beams Through Inmentioning

confidence: 99%

Section: Hadronic Jets In Active Galaxiesmentioning

confidence: 99%

Section: Propagation Of Relativistic Electron-proton Beams Through Inmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the Hadronic Beam Model for Gamma‐Ray Production in Blazars

Beall

Bednarek

1999

ApJ

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“…W 0 has been evaluated from R u = (U lm /U kT ) = 10-3 (n,,/r 3 )' / 2 (Rose et al 1987), where U kT = n e kT, and…”

Section: Scenario and Acceleration Ratesmentioning

confidence: 99%

Weightiness of the Dispersive Rate in Stochastic Acceleration Processes

Pérez‐Peraza¹,

Gallegos-Cruz²

1994

International Astronomical Union Colloquium

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We present analytical solutions to the transport equation of the accelerated particles that are valid over the entire energy range (nonrelativistic, transrelativistic, and ultrarelativistic) for the time-dependent and equilibrium cases. On the basis of these overall spectra, we have studied the relative importance of the term of average (systematic) energy increase and the term of diffusion (spread) in energy that define the evolution of accelerated particles within the frame of a simplified diffusion-convection transport equation, when the particle distribution function N(E, t) is assumed to be independent of spatial pitch-angle diffusion (isotropic). Since in some astrophysical works, only the term of average energy increase in the simplified transport equation in energy space is considered to be leading directly to a power-law-type spectrum, we have established the conditions under which such an approximation may be justified. The analysis is illustrated for acceleration by two different kinds of turbulence: MHD and Langmuir waves. The omission of the term of energy spread leads, in general, to an important depletion or overproduction of the accelerated particle flux that must be seriously considered in any calculation of the flux of secondary radiation produced by the accelerated particles. The presented analytical spectra may be of particular relevance to gamma-ray, neutron, and pion production in solar flares as well as in other astrophysical sites.

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How do Jets Establish Themselves ?

Sol¹,

Pelletier²

1992

Physics of Active Galactic Nuclei

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Radiation from relativistic beams interacting with interstellar gas

Cited by 19 publications

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On the Hadronic Beam Model for Gamma‐Ray Production in Blazars

On the Hadronic Beam Model for Gamma‐Ray Production in Blazars

Weightiness of the Dispersive Rate in Stochastic Acceleration Processes

How do Jets Establish Themselves ?

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