The Deutsch field gamma-ray pulsar — I. The model basics

Higgins, M. G.; Henriksen, R. N.

doi:10.1093/mnras/292.4.934

Cited by 12 publications

(18 citation statements)

References 9 publications

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“…The most striking feature of these νF ν plots is the flux peak above 0.1 GeV with a turnover at several GeV. Various models [21,22,23,24,25,26] conclude that these photons are emitted by the electrons or positrons accelerated above 5 TeV via curvature process. Such ultra-relativistic particles could also cause inverse-Compton (IC) scatterings.…”

Section: Gamma-ray Observations and Physical Processesmentioning

confidence: 97%

High-Energy Emission From Pulsar Magnetospheres

Hirotani

2006

Mod. Phys. Lett. A

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A synthesis of the present knowledge on gamma-ray emission from the magnetosphere of a rapidly rotating neutron star is presented, focusing on the electrodynamics of particle accelerators. The combined curvature, synchrotron, and inverse-Compton emission from ultra-relativistic positrons and electrons, which are created by two-photon and/or one-photon pair creation processes, or emitted from the neutron-star surface, provide us with essential information on the properties of the accelerator -electric potential drop along the magnetic field lines. A new accelerator model, which is a mixture of traditional inner-gap and outer gap models, is also proposed, by solving the Poisson equation for the electrostatic potential together with the Boltzmann equations for particles and gamma-rays in the two-dimensional configuration and twodimensional momentum spaces.

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Section: Gamma-ray Observations and Physical Processesmentioning

confidence: 97%

High-Energy Emission From Pulsar Magnetospheres

Hirotani

2006

Mod. Phys. Lett. A

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“…This pulsar gap model has been adapted to Kerr-Newman black holes (Punsly 1998). Even though other pair creation models have proven to have better predictive power for γ-ray emission than Chen & Ruderman (1993), such as Higgins & Henriksen (1997), it is beyond the burden and scope of this paper to compare and contrast the different gap models. This is already actively debated in the literature (see the references in the Introduction).…”

Section: D2 Curvature Radiation Based Gap Modelsmentioning

confidence: 99%

A new solution to the plasma starved event horizon magnetosphere

Punsly

Hardcastle

Hada

2018

A&A

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Very Long Baseline Interferometry observations at 86 GHz reveal an almost hollow jet in M87 with a forked morphology. The detailed analysis presented here indicates that the spectral luminosity of the central spine of the jet in M87 is a few percent of that of the surrounding hollow jet 200-400 µ as from the central black hole. Furthermore, recent jet models indicate that a hollow "tubular" jet can explain a wide range of plausible broadband spectra originating from jetted plasma located within ∼30 µ as of the central black hole, including the 230 GHz correlated flux detected by the Event Horizon Telescope. Most importantly, these hollow jets from the inner accretion flow have an intrinsic power capable of energizing the global jet out to kiloparsec scales. Thus motivated, this paper considers new models of the event horizon magnetosphere (EHM) in low luminosity accretion systems. Contrary to some models, the spine is not an invisible powerful jet. It is an intrinsically weak jet. In the new EHM solution, the accreted poloidal magnetic flux is weak and the background photon field is weak. It is shown how this accretion scenario naturally results in the dissipation of the accreted poloidal magnetic flux in the EHM not the accumulation of poloidal flux required for a powerful jet. The new solution indicates less large scale poloidal magnetic flux (and jet power) in the EHM than in the surrounding accretion flow and cannot support significant EHM driven jets.

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“…Whilst this approach has its merits in interpreting the data, it is unable to explain the intrinsic origin of this abrupt fall of the γ-ray radiated power with frequency, and this disappearance in the TeV range. Instead we must address directly the dynamics of the pulsar magnetosphere, as it was done in the Higgins & Henriksen's seminal papers [6,7], requiring improvement, since they used a classical single particle approach without going beyond the classical description, and they do not take into account properly the required influence of the radiation in the particle motion as we do in this paper.…”

Section: Introductionmentioning

confidence: 99%

“…For simplicity here, we shall assume that the typical 'relaxation time' will be the plasma period. Given the magnitude of the EM fields, a cold plasma approach is an acceptable one, with a close analogy with the single (test) particle approach, due to the formal equivalence between the Vlasov equation and standard orbit theory [17], as seen in [6,7,[18][19][20][21][22][23][24].…”

Section: Introductionmentioning

confidence: 99%

“…As accelerated charged particles radiate, the higher the particle energy, the higher the frequency of the radiated photons, and the particle power radiated, the Larmor power, creating a braking force, the Dirac force. Such force must be taken into account in the equation of motion, (contrary to what was done in [6,7]) and this is done classically substituting the usual Lorentz equation by the one known as the Lorentz-Dirac equation of motion (L-DEM) [25],…”

Section: Introductionmentioning

confidence: 99%

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Pulsar electrodynamics: Relativistic kinetic theory of radiative plasmas—collective phenomena and their radiation

et al. 2011

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The classical modelling of radiation by accelerated charged particles in pulsars predicts a cutoff in photon energy at around 25GeV. Whilst this is broadly consistent with observations, the classical treatment is not self-consistent, and cannot be extended to explain the rare high-energy detections of photons in the 100s of GeV range. In this paper we revisit the theoretical modelling of high-energy radiation processes in very strong electromagnetic fields, in the context of both single particles and collective plasmas. There are no classical constraints on this description. We find that there is indeed a critical energy of around 50 GeV that arises naturally in this self-consistent treatment, but rather than being a cutoff , this critical energy signals a transition from radiation that is classical to a quasi-quantum description, in which the particle is able to radiate almost its total energy in a single event. This new modelling therefore places pulsar radiation processes on a more secure physical basis, and admits the possibility of the production of TeV photons in a self-consistent way.

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The Deutsch field gamma-ray pulsar — I. The model basics

Cited by 12 publications

References 9 publications

High-Energy Emission From Pulsar Magnetospheres

High-Energy Emission From Pulsar Magnetospheres

A new solution to the plasma starved event horizon magnetosphere

Pulsar electrodynamics: Relativistic kinetic theory of radiative plasmas—collective phenomena and their radiation

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