Trapped Positrons and Electrons in the Inner Radiation Belt According to Data of the PAMELA Experiment

M. Ricci; S. B. Ricciarini; M. F. Runtso; M. Simon; R. Sparvoli; P. Spillantini; Y. I. Stozhkov; Y. T. Yurkin; V. V. Mikhailov; O. Adriani; G. A. Bazilevskaya; G. C. Barbarino; R. Bellotti; E. A. Bogomolov; M. Boezio; V. Bonvicini; M. Bongi; S. Bottai; A. Bruno; A. Vacchi; E. Vannuccini; G. I. Vasilyev; S. A. Voronov; A. M. Galper; C. De Santis; V. Di Felice; G. Zampa; N. Zampa; M. Casolino; D. Campana; A. V. Karelin; P. Carlson; G. Castellini; F. Cafagna; A. A. Kvashnin; A. N. Kvashnin; S. V. Koldashov; S. A. Koldobskiy; S. Y. Krutkov; A. A. Leonov; A. G. Mayorov; V. V. Malakhov; M. Martucci; L. Marcelli; W. Menn; M. Merge; Yu. V. Mikhailova; E. Mocchiutti; A. Monaco; N. Mori; R. Munini; G. Osteria; B. Panico; P. Papini; P. Picozza; M. Pearce

doi:10.1134/S1063778818040129

Trapped Positrons and Electrons in the Inner Radiation Belt According to Data of the PAMELA Experiment

作者: Ricci M.¹, Ricciarini S.B.², Runtso M.F.³, Simon M.⁴, Sparvoli R.⁵^,6, Spillantini P.³, Stozhkov Y.I.⁷, Yurkin Y.T.³, Mikhailov V.V.³, Adriani O.⁸^,2, Bazilevskaya G.A.⁷, Barbarino G.C.⁶^,9, Bellotti R.¹⁰^,11, Bogomolov E.A.¹², Boezio M.¹³, Bonvicini V.¹³, Bongi M.⁸^,2, Bottai S.², Bruno A.¹⁰^,11, Vacchi A.¹³^,14, Vannuccini E.², Vasilyev G.I.¹², Voronov S.A.³, Galper A.M.³, De Santis C.⁵^,6, Di Felice V.⁵^,15, Zampa G.¹³, Zampa N.¹³, Casolino M.⁵, Campana D.⁹, Karelin A.V.³, Carlson P.¹⁶, Castellini G.¹⁷, Cafagna F.¹¹, Kvashnin A.A.⁷, Kvashnin A.N.⁷, Koldashov S.V.³, Koldobskiy S.A.³, Krutkov S.Y.¹², Leonov A.A.³, Mayorov A.G.³, Malakhov V.V.³, Martucci M.⁶^,1, Marcelli L.⁶, Menn W.⁴, Merge M.⁵^,6, Mikhailova Y.V.³, Mocchiutti E.¹³, Monaco A.¹⁰^,11, Mori N.², Munini R.¹³^,6, Osteria G.⁹, Panico B.⁹, Papini P.², Picozza P.⁵^,6, Pearce M.¹⁶
隶属关系:
1. Istituto Nazionale di Fisica Nucleare
2. Istituto Nazionale di Fisica Nucleare, Sezione di Firenze
3. National Research Nuclear University MEPhI
4. Department Physik
5. Istituto Nazionale di Fisica Nucleare, “Tor Vergata”
6. Dipartimento di Fisica
7. Lebedev Physical Institute
8. Dipartimento di Fisica, Piazza S. Marco 4
9. Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Strada Comunale Cintia
10. Dipartimento di Fisica, Piazza Umberto I
11. Istituto Nazionale di Fisica Nucleare, Sezione di Bari
12. Ioffe Physical-Technical Institute
13. Istituto Nazionale di Fisica Nucleare, Sezione di Trieste
14. Dipartimento di Scienze Matematiche, Informatiche e Fisiche (DMIF)
15. Agenzia Spaziale Italiana (ASI) Science Data Center, Via del Politecnico, snc, Edificio D
16. KTH Royal Institute of Technology, Dipartimento di Fisica, and the Oskar Klein Centre for Cosmoparticle Physics
17. Istituto di Fisica Applicata “Nello Carrara”
期: 卷 81, 编号 4 (2018)
页面: 515-519
栏目: Elementary Particles and Fields
URL: https://journals.rcsi.science/1063-7788/article/view/194367
DOI: https://doi.org/10.1134/S1063778818040129
ID: 194367

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Measurements of secondary-electron and secondary-positron fluxes below the geomagnetic cutoff in near-Earth space were performed by means of the PAMELA magnetic spectrometer installed on board the Resurs-DK1 satellite launched on June 15, 2006, in an elliptical orbit of inclination 70° and altitude 350 to 600 km. This spectrometer permits measuring the fluxes of electrons and positrons over a wide energy range, as well as determining their spatial distributions to a precision of about 2°. A calculation of particle trajectories in the geomagnetic field makes it possible to separate electrons and positrons originating from cosmic-ray interactions in the Earth’s magnetosphere. The spatial distributions of quasitrapped, trapped, and short-lived albedo positrons and electrons of energy above 70 MeV in the radiation belt were analyzed. The ratio of the electron-to-positron fluxes and the energy spectra of the electrons and positrons in question are indicative of different productionmechanisms for stably trapped and quasitrapped secondary particles.

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Trapped Positrons and Electrons in the Inner Radiation Belt According to Data of the PAMELA Experiment

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