Compton and Thomson scattering in strong magnetic fields

Herold, H.

doi:10.1103/physrevd.19.2868

Cited by 212 publications

(221 citation statements)

References 15 publications

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“…There is also enhancement for oblique initial photon angles in the energy region 0 < ω ′ ∼ < ω ′ GE /2. At the lowest frequencies, Figure 6 compares favourably with the results of Herold (1979) and Daugherty and Harding (1986) Figure 10.) The PC resonances are within the range of energies considered in Figure 7 and are particularly apparent in Figure 7(b).…”

Section: Resultssupporting

confidence: 66%

“…The choice of these wave functions, specifically the the magnetic moment operator as the spin operator, is strongly preferred over the Johnson and Lippmann (JL) wave functions, used by Gonthier et al (2000). In particular, it is only for this choice of spin operator that the spin eigenvalue is a constant of the motion (Sokolov and Ternov (1968); Herold (1979); Melrose and Parle (1983)). Further, the JL wave functions lack symmetry between the electron and positron states.…”

Section: Choice Of Wave Functionsmentioning

confidence: 99%

“…The PC resonance is associated with the second Feynman diagram, in which the intermediate particle is a positron. Both of these resonances were identified as far back as 1979 by Herold (1979), who restricted his calculations to photon energies below the first PC threshold. At either a GA or a PC resonance the question arises as to whether the process should be regarded as a second-order process, corresponding to Compton scattering with a virtual intermediate state, or as a 2-step process, corresponding to two first-order processes with a real intermediate state.…”

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confidence: 99%

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Resonant Compton scattering associated with pair creation

Weise

2014

Astrophys Space Sci

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Studies of Compton scattering by relativistic electrons in a strong magnetic field have been restricted to either incident photon angles θ ′ aligned along the magnetic field B or incident photon energies ω ′ below the first pair creation threshold ω ′ P C . When these restrictions are relaxed there is a resonance in Compton scattering associated with pair creation (PC), that is analogous to but independent of known resonances associated with gyromagnetic absorption (GA). As with the GA resonances, that may be labeled by the Landau quantum numbers of the relevant states, there is a sequence of PC resonances where the scattering cross section diverges. In this paper, the lowest divergence is studied for incident photon energies satisfying ω ′ 2 sin 2 θ ′ /(2eB) ≪ 1, assuming that the scattering electron is in its ground (Landau) state. This lowest resonance affects only parallel-polarized photons.

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Section: Resultssupporting

confidence: 66%

Section: Choice Of Wave Functionsmentioning

confidence: 99%

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confidence: 99%

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Resonant Compton scattering associated with pair creation

Weise

2014

Astrophys Space Sci

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“…Two main radiation processes considered here that can produce pairs are resonant inverse Compton scattering (RICS) (Herold 1979;Gonthier et al 2000) and curvature radiation. RICS occurs at ε B ∼ ε th γ in the rest frame.…”

Section: The Acceleration Efficiency Limited By Pair Productionmentioning

confidence: 99%

High energy neutrinos from fast spinning magnetars

Luo

2005

Astroparticle Physics

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Fast spinning magnetars are discussed as strong sources of high energy neutrinos. Pulsars may be born with a short rotation period of milliseconds with the magnetic field amplified through dynamo processes up to ∼ 10 15 − 10 16 G. As such millisecond magnetars (MSMs) have an enormous spin-down power ∼ 10 50 erg s −1 , they can be potentially a strong, extragalactic high-energy neutrino source. Specifically, acceleration of ions and subsequent photomeson production within the MSM magnetosphere are considered. As in normal pulsars, particle acceleration leads to electron-positron pair cascades that constrains the acceleration efficiency. The limit on the neutrino power as a fraction of the spin-down power is calculated. It is shown that neutrinos produced in the inner magnetosphere have characteristic energy about a few ×100 GeV due to the constraint of cooling of charged pions through inverse Compton scattering. TeV neutrinos may be produced in the outer magnetosphere where ions can be accelerated to much higher energies and the pion cooling is less severe than in the inner magnetosphere. High energy neutrinos can also be produced from interactions between ultra-high energy protons accelerated in the magnetosphere and a diffuse thermal radiation from the ejecta or from the interaction region between the MSM wind and remnant shell. The detectability of neutrinos in the early spin-down phase by the current available and planned neutrino detectors is discussed.

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“…These errors have no effect on the results presented in the paper. I have taken this opportunity to discuss a controversy concerning different frequency factors that appear in the expressions for the cross sections: in Weise (2014) there is a factor (ω/ω ) 2 , whereas in Daugherty and Harding (1986), Herold (1979) and Gonthier et al (2000) the corresponding factor is ω/ω . …”

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confidence: 99%

Erratum to: Resonant Compton scattering associated with pair creation

Weise

2015

Astrophys Space Sci

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I correct typographical errors in the paper Weise (2014). These errors have no effect on the results presented in the paper. I have taken this opportunity to discuss a controversy concerning different frequency factors that appear in the expressions for the cross sections: in Weise (2014) there is a factor (ω/ω ) 2 , whereas in Daugherty and Harding (1986), Herold (1979) and Gonthier et al. (2000) the corresponding factor is ω/ω . Typographical errorsThere are three equations in Sect. 2.3 which have typographical errors. The first equation is Eq. (24), the left hand side of which should have the subscript MM in the same manner that Eq. (22) does. Consequently, Eq. (24) should read as follows:The

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Compton and Thomson scattering in strong magnetic fields

Cited by 212 publications

References 15 publications

Resonant Compton scattering associated with pair creation

Resonant Compton scattering associated with pair creation

High energy neutrinos from fast spinning magnetars

Erratum to: Resonant Compton scattering associated with pair creation

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