The May 17, 2012 solar event: back-tracing analysis and flux reconstruction with PAMELA

International Conference on Particle Physics and Astrophysics

Bruno, A.^1 ; Adriani, O.^2,3 ; Barbarino, G.C.^4,5 ; Bazilevskaya, G.A.^6 ; Bellotti, R.^1,7 ; Boezio, M.^8 ; Bogomolov, E.A.^9 ; Bongi, M.^2,3 ; Bonvicini, V.^8 ; Bottai, S.^3 ; Bravar, U.^10 ; Cafagna, F.^7 ; Campana, D.^5 ; Carbone, R.^8 ; Carlson, P.^11 ; Casolino, M.^12,13 ; Castellini, G.^14 ; Christian, E.C.^15 ; De Donato, C.^12,17 ; De Nolfo, G.A.^15 ; De Santis, C.^12,17 ; De Simone, N.^12 ; Felice, V. Di^12,18 ; Formato, V.^8,19 ; Galper, A.M.^16 ; Karelin, A.V.^16 ; Koldashov, S.V.^16 ; Koldobskiy, S.^16 ; Krutkov, S.Y.^9 ; Kvashnin, A.N.^6 ; Lee, M.^10 ; Leonov, A.^16 ; Malakhov, V.^16 ; Marcelli, L.^12,17 ; Martucci, M.^17,20 ; Mayorov, A.G.^16 ; Menn, W.^21 ; Mergè, M.^12,17 ; Mikhailov, V.V.^16 ; Mocchiutti, E.^8 ; Monaco, A.^1,7 ; Mori, N.^2,3 ; Munini, R.^8,19 ; Osteria, G.^5 ; Palma, F.^12,17 ; Panico, B.^5 ; Papini, P.^3 ; Pearce, M.^11 ; Picozza, P.^12,17 ; Ricci, M.^20 ; Ricciarini, S.B.^3,14 ; Ryan, J.M.^10 ; Sarkar, R.^22,23 ; Scotti, V.^4,5 ; Simon, M.^21 ; Sparvoli, R.^12,17 ; Spillantini, P.^2,3 ; Stochaj, S.^24 ; Stozhkov, Y.I.^6 ; Vacchi, A.^8 ; Vannuccini, E.^3 ; Vasilyev, G.I.^9 ; Voronov, S.A.^16 ; Yurkin, Y.T.^16 ; Zampa, G.^8 ; Zampa, N.^8 ; Zverev, V.G.^16

Department of Physics, University of Bari Aldo Moro, Bari

I-70126, Italy^1

Department of Physics and Astronomy, University of Florence, Sesto Fiorentino Florence

I-50019, Italy^2

INFN, Sezione di Florence, Sesto Fiorentino Florence

I-50019, Italy^3

Department of Physics, University of Naples Federico II, Naples

I-80126, Italy^4

INFN, Sezione di Naples, Naples

I-80126, Italy^5

P.N. Lebedev Physical Institute, Russian Academy of Sciences, Moscow

RU-119991, Russia^6

INFN, Sezione di Bari, Bari

I-70126, Italy^7

INFN, Sezione di Trieste, Trieste

I-34149, Italy^8

Ioffe Physical Technical Institute, St.-Petersburg

RU-194021, Russia

(10) Space Science Center, University of New Hampshire, Durham

NH, United States

(11) KTH, Department of Physics, Oskar Klein Centre for Cosmoparticle Physics, AlbaNova University Centre, Stockholm

SE-10691, Sweden

(12) INFN, Sezione di Rome Tor Vergata, Rome

I-00133, Italy

(13) RIKEN, Advanced Science Institute, Wako-shi Saitama, Japan

(14) IFAC, Sesto Fiorentino Florence

I-50019, Italy

(15) Heliophysics Division, NASA Goddard Space Flight Ctr, Greenbelt

MD, United States

(16) National Research Nuclear University MEPhI, Moscow Engineering Physics Institute), Kashirskoye highway 31, Moscow

RU-115409, Russia

(17) Department of Physics, University of Rome Tor Vergata, Rome

I-00133, Italy

(18) Agenzia Spaziale Italiana (ASI), Science Data Center, Rome

I-00133, Italy

(19) Department of Physics, University of Trieste, Trieste

I-34147, Italy

(20) INFN, Laboratori Nazionali di Frascati, Frascati

I-00044, Italy

(21) Department of Physics, Universitat Siegen, Siegen

D-57068, Germany

(22) Indian Centre for Space Physics, 43 Chalantika, Kolkata West-Bengal

700084, India

(23) Previously at INFN, Sezione di Trieste, Trieste

I-34149, Italy

(24) Electrical and Computer Engineering, New Mexico State University, Las Cruces

NM, United States^9

关键词: Asymptotic directions;    Direct observations;    Earth's magnetosphere;    Flux reconstruction;    Ground level enhancements;    Interplanetary magnetic fields;    Solar energetic particles;    World-wide networks;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/675/3/032006/pdf
DOI  :  10.1088/1742-6596/675/3/032006

来源: IOP

【 摘 要 】

The PAMELA space experiment is providing first direct observations of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth orbit, bridging the low energy measurements by other spacecrafts and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies associated to SEP events. The analysis is supported by an accurate back-tracing simulation based on a realistic description of the Earth's magnetosphere, which is exploited to estimate the SEP energy spectra as a function of the asymptotic direction of arrival with respect to the Interplanetary Magnetic Field (IMF). In this work we report the results for the May 17, 2012 event.