Measurement of the flux of primary cosmic ray antiprotons with energies of 60 MeV to 350 GeV in the PAMELA experiment

O. Adriani, G. A. Bazilevskaya, G. C. Barbarino, R. Bellotti, M. Boezio, E. A. Bogomolov, V. Bonvicini, M. Bongi, L. Bonechi, S. V. Borisov, S. Bottai, A. Bruno, A. Vacchi, E. Vannuccini, G. I. Vasilyev, S. A. Voronov, J. Wu, A. M. Galper, L. A. Grishantseva, I. A. DanilchenkoW. Gillard, G. Jerse, G. Zampa, N. Zampa, V. G. Zverev, M. Casolino, D. Campana, R. Carbone, A. V. Karelin, P. Carlson, G. Castellini, F. Cafagna, A. N. Kvashnin, S. V. Koldashov, S. A. Koldobskiy, S. Y. Krutkov, L. Consiglio, A. A. Leonov, A. G. Mayorov, V. V. Malakhov, W. Malvezzi, L. Marcelli, W. Menn, V. V. Mikhailov, E. Mocchiutti, A. Monaco, N. Mori, N. N. Nikonov, G. Osteria, F. Palma, P. Papini, C. Pizzolotto, M. P. de Pascale, P. Picozza, M. Pearce, M. Ricci, S. Ricciarini, L. Rossetto, M. F. Runtso, C. De Santis, R. Sarkar, M. Simon, N. De Simone, R. Sparvoli, P. Spillantini, Y. I. Stozhkov, V. Di Felice, Y. T. Yurkin

Research output: Contribution to journalArticlepeer-review

119 Scopus citations


It is interesting to measure the antiproton galactic component in cosmic rays in order to study the mechanisms by which particles and antiparticles are generated and propagate in the Galaxy and to search for new sources of, e. g., annihilation or decay of dark matter hypothetical particles. The antiproton spectrum and the ratio of the fluxes of primary cosmic ray antiprotons to protons with energies of 60 MeV to 350 GeV found from the data obtained from June 2006 to January 2010 in the PAMELA experiment are presented. The usage of the advanced data processing method based on the data classification mathematical model made it possible to increase statistics and analyze the region of higher energies than in the earlier works.

Original languageEnglish
Pages (from-to)621-627
Number of pages7
JournalJETP Letters
Issue number10
StatePublished - 2013
Externally publishedYes

Bibliographical note

Funding Information:
We are grateful to the Space Council of the Russian Academy of Sciences, Russian Federal Space Agency Roscosmos, State Research and Production Space Rocket Center Progress, Research Center for Earth Operative Monitoring, Italian Space Agency, Deut sches Zentrum für Luft und Raumfahrt, Swedish National Space Board, and Swedish Research Council.


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