Multi-particle analysis of the december 13th 2006 forbush decrease with PAMELA experiment

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

In this paper we present PAMELA multi-particle observation of the Forbush decrease (FD) following the December 13th 2006 solar particle event. The FD is the sudden decrease of the galactic cosmic ray flux due to the transit of a Coronal Mass Ejection (CME). The satellite-borne experiment PAMELA on-board Resurs-DK1 satellite and consist of a magnetic spectrometer with time-of-flight and calorimeter detectors. PAMELA can study in real time with high precision the temporal and energetic evolution of several particle fluence during and after crossing of the magnetic cloud generated by the CME. The effect is stronger than what detected on ground with neutron monitor. With flux reduction can be as high as 30% decreasing at 1.5GV. No difference of the FD has been found for different particles proving that there is no charge sign dependence of FD for this event.

Multi-particle analysis of the december 13th 2006 forbush decrease with PAMELA experiment / Merge M.; Casolino M.; Adriani O.; Barbarino G.C.; Bazilevskaya G.A.; Bellotti R.; Boezio M.; Bogomolov E.A.; Bongi M.; Bonvicini V.; Bottai S.; Bruno A.; Cafagna F.; Campana D.; Carbone R.; Carlson P.; Castellini G.; Danilchenko I.A.; Donato C.D.E.; Santis C.D.E.; Simone N.D.E.; Felice V.D.I.; Formato V.; Galper A.M.; Karelin A.V.; Koldashov S.V.; Koldobskiy S.; Krutkov S.Y.; Kvashnin A.N.; Leonov A.; Malakhov V.; Marcelli L.; Martucci M.; Mayorov A.G.; Menn W.; Mikhailov V.V.; Mocchiutti E.; Monaco A.; Mori N.; Munini R.; Osteria G.; Palma F.; Papini P.; Pearce M.; Picozza P.; Pizzolotto C.; Ricci M.; Ricciarini S.B.; Sarkar R.; Simon M.; Scotti V.; Sparvoli R.; Spillantini P.; Stozhkov Y.I.; Vacchi A.; Vannuccini E.; Vasilyev G.; Voronov S.A.; Yurkin Y.T.; Zampa G.; Zampa N.; Zverev V.G.. - ELETTRONICO. - 2013-:(2013), pp. 0-0. ( 33rd International Cosmic Rays Conference, ICRC 2013 bra 2013).