PAMELA was launched on June 15th 2006 on board the Russian Resurs-DK1 satellite. The satellite is flying in high inclination (70o), low Earth Orbit (350-600 km), performing measurements in different points and conditions of the geomagnetosphere. It is a multi-purpose apparatus composed of a permanent magnet spectrometer to provide particle charge, rigidity and incoming angle. A series of six scintillator counters arranged at its extremities provide redundant Time-of-Flight and charge data. Lepton/ hadron identification is performed by a Silicon-Tungsten calorimeter and a Neutron detector placed at the bottom of the device. An Anticounter system is used offline to reject false triggers coming from the satellite. PAMELA is capable of detecting protons (80 MeV- 700 GeV), antiprotons (80 MeV-190 GeV), electrons (50 MeV - 400 GeV), positrons (50 MeV - 270 Gev) and nuclei (≃ 100 MeV/n - 200GeV/nuc ). In addition, a technique employing scintillator counting rate and range energy methods allows to lower the minimum detectable energy range to 36 MeV and 3.5 MeV for protons and electrons respectively. The orbit of the satellite and the characteristics of the magnet spectrometer allow PAMELA to perform a very detailed measurement of the nature and spectra of primary (above cutoff) and secondary particles (sub-cutoff: trapped, reentrant albedo, etc.). The precise measurements of particle distribution in different regions of the orbit provides information on the processes of production, propagation and interaction of particles in Earth’s magnetosphere. In this work we present some measurements of galactic and secondary particles performed in the first months of operation.
Observations of primary, trapped and quasi trapped particles with PAMELA experiment / Casolino, M.; Adriani, O.; Ambriola, M.; Barbarino, G.C.; Basili, A.; Bazilevskaja, G.A.; Bellotti, R.; Boezio, M.; Bogomolov, E.A.; Bonechi, L.; Bongi, M.; Bongiorno, L.; Bonvicini, V.; Bruno, A.; Cafagna, F.; Campana, D.; Carlson, P.; Castellini, G.; De Marzo, C.; Conrad, J.; De Pascale, M.P.; De Rosa, G.; Di Felice, V.; Fedele, D.; Galper, A.M.; Hofverberg, P.; Koldashov, S.V.; Krutkov, S.Yu.; Kvashnin, A.N.; Lundquist, J.; Maksumov, O.; Malvezzi, V.; Marcelli, L.; Menn, W.; Mikhailov, V.V.; Minori, M.; Misin, S.; Mocchiutti, E.; Morselli, A.; Nikonov, N.N.; Orsi, S.; Osteria, G.; Papini, P.; Pearce, M.; Picozza, P.; Ricci, M.; Ricciarini, S.B.; Runtso, M.F.; Russo, S.; Simon, M.; Sparvoli, R.; Spillantini, P.; Stozhkov, Yu.I.; Taddei, E.; Vacchi, A.; Vannuccini, E.; Vasilyev, G.; Voronov, S.A.; Yurkin, Y.T.; Zampa, G.; Zampa, N.; Zverev, V.G.. - ELETTRONICO. - 1:(2007), pp. 709-712. (Intervento presentato al convegno 30th International Cosmic Ray Conference, ICRC 2007 tenutosi a Merida, Yucatan, mex nel 2007).
Observations of primary, trapped and quasi trapped particles with PAMELA experiment
ADRIANI, OSCAR;BONGI, MASSIMO;
2007
Abstract
PAMELA was launched on June 15th 2006 on board the Russian Resurs-DK1 satellite. The satellite is flying in high inclination (70o), low Earth Orbit (350-600 km), performing measurements in different points and conditions of the geomagnetosphere. It is a multi-purpose apparatus composed of a permanent magnet spectrometer to provide particle charge, rigidity and incoming angle. A series of six scintillator counters arranged at its extremities provide redundant Time-of-Flight and charge data. Lepton/ hadron identification is performed by a Silicon-Tungsten calorimeter and a Neutron detector placed at the bottom of the device. An Anticounter system is used offline to reject false triggers coming from the satellite. PAMELA is capable of detecting protons (80 MeV- 700 GeV), antiprotons (80 MeV-190 GeV), electrons (50 MeV - 400 GeV), positrons (50 MeV - 270 Gev) and nuclei (≃ 100 MeV/n - 200GeV/nuc ). In addition, a technique employing scintillator counting rate and range energy methods allows to lower the minimum detectable energy range to 36 MeV and 3.5 MeV for protons and electrons respectively. The orbit of the satellite and the characteristics of the magnet spectrometer allow PAMELA to perform a very detailed measurement of the nature and spectra of primary (above cutoff) and secondary particles (sub-cutoff: trapped, reentrant albedo, etc.). The precise measurements of particle distribution in different regions of the orbit provides information on the processes of production, propagation and interaction of particles in Earth’s magnetosphere. In this work we present some measurements of galactic and secondary particles performed in the first months of operation.
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