Polarization for pair annihilation in strong magnetic fields

Semionova, L.; Leahy, D. A.

doi:10.1051/aas:2000102

Cited by 6 publications

(7 citation statements)

References 13 publications

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“…This was made possible by using the proper spin eigenfunctions for e − and e + in a strong magnetic field, as defined by Sokolov & Ternov (1983). Polarized pair annihilation rates have presented in Semionova & Leahy (2000), and polarized photon emission rates in Semionova & Leahy (1999). With the polarized pair creation attentuation coefficients presented here, one is one step closer to being able to properly study the polarizedphoton/ spin-polarized-e − −e + radiation transfer problem in strong magnetic fields.…”

Section: Discussionmentioning

confidence: 81%

Remarks concerning pair creation in strong magnetic fields

Semionova

Leahy

2001

A&A

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Abstract. We derive the probability and attenuation coefficients for pair creation in first order of polarized electrons and positrons. The positron and electron can occupy arbitrary Landau levels and the attenuation coefficient is evaluated for any direction and polarization of the photon. When we take θ = 90• and sum over polarization of the spins of the e + − e − pair, we obtain results which differ from the expressions for the attenuation coefficient obtained by Daugherty & Harding (1983), by the factor (1 + δN,0)(1 + δ N ,0 )/4, in agreement with Frangodimitraki-Georgiadou (1991).

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Section: Discussionmentioning

confidence: 81%

Remarks concerning pair creation in strong magnetic fields

Semionova

Leahy

2001

A&A

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“…However, the effectiveness of synchrotron cooling may keep the densities of excited states low enough relative to the ground state to cancel the increase in the annihilation rate. The one-photon annihilation rate for different photon polarizations and particle spin states has been derived by Wunner et al (1986) and Semionova & Leahy (2000).…”

Section: Pair Production and Annihilationmentioning

confidence: 99%

Physics of strongly magnetized neutron stars

Harding¹,

Lai²

2006

Rep. Prog. Phys.

820

763

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Abstract. There has recently been growing evidence for the existence of neutron stars possessing magnetic fields with strengths that exceed the quantum critical field strength of 4.4 × 10 13 G, at which the cyclotron energy equals the electron rest mass. Such evidence has been provided by new discoveries of radio pulsars having very high spin-down rates and by observations of bursting gamma-ray sources termed magnetars. This article will discuss the exotic physics of this high-field regime, where a new array of processes becomes possible and even dominant, and where familiar processes acquire unusual properties. We review the physical processes that are important in neutron star interiors and magnetospheres, including the behavior of free particles, atoms, molecules, plasma and condensed matter in strong magnetic fields, photon propagation in magnetized plasmas, free-particle radiative processes, the physics of neutron star interiors, and field evolution and decay mechanisms. Application of such processes in astrophysical source models, including rotation-powered pulsars, soft gamma-ray repeaters, anomalous X-ray pulsars and accreting X-ray pulsars will also be discussed. Throughout this review, we will highlight the observational signatures of high magnetic field processes, as well as the theoretical issues that remain to be understood.

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“…where the quantities N (1,2) can be found for example in [3] and [7]. It is worth stressing here that N (1,2) depend on photon polarizations r 1 and r 2 .…”

Section: Theorymentioning

confidence: 95%

“…The exact form of the solutions can be found e.g. in [7]. Here we only stress that the components of the bispinors contain oscillator wave functions for n-th Landau level, for which the energy equals E n = m 2 0 + p 2 + 2n/λ 2 (we have dened λ ≡ (m 0 √ b) −1 and b ≡ B/B 0 ).…”

Section: Theorymentioning

confidence: 99%

See 1 more Smart Citation

Electron-Positron Annihilation in Ultra-Strong Magnetic Fields. Comparison of One- and Two-Photon Annihilation at Middly Relativistic Regime

Lewicka

2014

Acta Phys. Pol. A

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We consider the one-and two-photon e + e − annihilation processes in an ultra-strong magnetic eld, at middly relativistic regime. Such conditions are reached in neutron stars and especially in magnetars, where electrons and positrons ow within the magnetar corona with average momenta of the order of p ∼ m0c, where m0 electron mass, c light speed. We pay special attention to the ratio of the total annihilation rates of both processes. The well-known result is that in the limit p → 0 and for magnetic induction above the critical Schwinger value B0 = 4.41×10 9 T, one-photon annihilation dominates over the two-photon process. Results presented in this article verify the current knowledge about this ratio in magnetars; the calculations indicate that for particles moving with middly relativistic momenta both processes can be equally important.

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Polarization for pair annihilation in strong magnetic fields

Cited by 6 publications

References 13 publications

Remarks concerning pair creation in strong magnetic fields

Remarks concerning pair creation in strong magnetic fields

Physics of strongly magnetized neutron stars

Electron-Positron Annihilation in Ultra-Strong Magnetic Fields. Comparison of One- and Two-Photon Annihilation at Middly Relativistic Regime

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