On Energy and Angular Distributions of Electrons in Triplet Production

Haug, E.

doi:10.1515/zna-1985-1202

Cited by 7 publications

(7 citation statements)

References 11 publications

(36 reference statements)

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“…Maximon and Gimm (1981) provided new and simplified expressions for the recoil distribution in triplet production, from which Gimm (1982), using the same Hubbell et al non-relativistic S(x,Z) values as used in HGØ (1980), recomputed k e for all elements Z ¼ 12100 and all energies above 10 MeV, presenting his results compactly in the form of 7-parameter polynomial fits. Also, Haug (1985) re-examined the energy and angular distributions of electrons in triplet production, refining and simplifying the expressions of Jarp and Mork (1973). More recently, Haug (2004) has investigated the production of electron-positron pairs in a hot Maxwellian plasma at semirelativistc and relativistic temperatures, in the fields of positrons and electrons (triplet, k e ) and nuclei (k n ), of interest in astrophysics in the study of stellar black-hole binaries and Seyfert galaxies (see, e.g., Zdziarski, 1982;Lightman, 1982;Lightman and Zdziarski, 1987;Zdziarski et al, 1990;Mastichiadis et al, 1994).…”

Section: Some Further Theoretical Work Beyond Hgø (1980)mentioning

confidence: 99%

“…in which k e BG is the Borsellino (1947a, b)-Ghizzetti (1947 unscreened triplet cross section including retardation, the ratio k e H /k e BG uses the Haug (1975Haug ( , 1981Haug ( , 1985 results to include the g-e interaction and exchange effects, and the Dk e BH (scr) screening and electron-binding effects were computed according to the Bethe-Heitler (Wheeler-Lamb) expression, using the non-relativistic incoherent scattering functions S(x,Z) compiled by Hubbell et al (1975) from various available sources, and the triplet radiative correction factor 1.01, as advised by Mork (1967), is taken as this constant value over the entire energy range.…”

Section: Pair and Triplet Measurements: A Brief History And Surveymentioning

confidence: 99%

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Electron–positron pair production by photons: A historical overview

Hubbell

2006

Radiation Physics and Chemistry

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This account briefly traces the growth of our theoretical and experimental knowledge of electron-positron pair production by photons, from the prediction of the positron by Dirac [1928a can interact with the Coulomb field of an atomic nucleus to be transformed into an electron-positron pair, the probability increasing with increasing photon energy, up to a plateau at high energies, and increasing with increasing atomic number approximately as the square of the nuclear charge (proton number). This interaction can also take place in the field of an atomic electron, for photons of energy in excess of 4m e c 2 (2.044 MeV), in which case the process is called triplet production due to the track of the recoiling atomic electron adding to the tracks of the created electron-positron pair. The last systematic computations and tabulations of pair and triplet cross sections, which are the predominant contributions to the photon mass attenuation coefficient for photon energies 10 MeV and higher, were those of Hubbell et al. [Pair, triplet, and total atomic cross sections (and mass attenuation coefficients) for 1 MeV-100 GeV photons in elements Z ¼ 1-100. J. Phys. Chem. Ref. Data 9, 1023Data 9, -1147, from threshold (1.022 MeV) up to 100 GeV, for all elements Z ¼ 1-100. These computations required some ad hoc bridging functions between the available low-energy and high-energy theoretical models. Recently (1979Recently ( -2001, Sud and collaborators have developed some new approaches including using distorted wave Born approximation (DWBA) theory to compute pair production cross sections in the intermediate energy region (5.0-10.0 MeV) on a firmer theoretical basis. These and other recent developments, and their possible implications for improved computations of pair and triplet cross sections, are discussed. Published by Elsevier Ltd.

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Section: Some Further Theoretical Work Beyond Hgø (1980)mentioning

confidence: 99%

Section: Pair and Triplet Measurements: A Brief History And Surveymentioning

confidence: 99%

Electron–positron pair production by photons: A historical overview

Hubbell

2006

Radiation Physics and Chemistry

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“…The newest AMS data confirm this dependence with a slope of can be expected to throw light on these questions. (Haug 1975(Haug , 1981(Haug , 1985(Haug , 2004. So three leptons result from this process, hence the name.…”

Section: The Secondary Cosmic Ray Particlesmentioning

confidence: 99%

“…There is now evidence for an identical behavior of Lithium, Beryllium ). This is a process known as "triplet pair production", in which an energetic electron encounters a photon, and produces an extra electron-positron pair (Haug 1975(Haug , 1981(Haug , 1985(Haug , 2004. So three leptons result from this process, hence the name.…”

Section: The Secondary Cosmic Ray Particlesmentioning

confidence: 99%

Supernova explosions of massive stars and cosmic rays

Biermann

Tjus

Caramete

et al. 2018

Advances in Space Research

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Most cosmic ray particles observed derive from the explosions of massive stars. Massive stars from slightly above about 10 M explode as supernovae via a mechanism which we do not know yet: two not mutually exclusive main ideas are an explosion driven by neutrinos, or the magneto-rotational mechanism, in which the magnetic field acts like a conveyorbelt to transport energy outwards for an explosion. Massive stars above about 25 M , depending on their heavy element abundance, commonly produce stellar black holes in

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“…The case of electron-positron bremsstrahlung is considered in 28 . The differential cross section for the radiative pair production is obtained in 29 , while the total cross section is found in 30 . The three-photon annia) Electronic mail: nikprokopenya@gmail.com b) Electronic mail: i.siutsou@dragon.bas-net.by c) Electronic mail: veresh@icra.it hilation is studied in 31,32 .…”

Section: Introductionmentioning

confidence: 99%

Numerical Scheme for Treatment of Uehling–Uhlenbeck Equation for Binary and Triple Interactions in Relativistic Plasma

2018

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Binary interactions in relativistic plasma, such as Coulomb and Compton scattering as well as pair creation and annihilation are well known and studied in details. Triple interactions, namely relativistic bremsstrahlung, double Compton scattering, radiative pair production, triple pair production/annihilation and their inverse processes, are usually considered as emission processes in astrophysical problems, as well as in laboratory plasmas. Their role in plasma kinetics is fundamental 1. We present a new conservative scheme for computation of Uehling-Uhlenbeck collision integral for all triple interactions in relativistic plasma based on direct integration of exact QED matrix elements. Reaction rates for thermal distributions are compared, where possible, with the corresponding analytic expressions, showing good agreement. Our results are relevant for quantitative description of relativistic plasmas out of equilibrium, both in astrophysical and laboratory conditions.

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On Energy and Angular Distributions of Electrons in Triplet Production

Cited by 7 publications

References 11 publications

Electron–positron pair production by photons: A historical overview

Electron–positron pair production by photons: A historical overview

Supernova explosions of massive stars and cosmic rays

Numerical Scheme for Treatment of Uehling–Uhlenbeck Equation for Binary and Triple Interactions in Relativistic Plasma

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