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

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

doi:10.1134/s002136401222002x

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.

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. Danilchenko;W. 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;P. Picozza;M. Pearce;M. Ricci;S. Ricciarini;L. Rossetto;M. F. Runtso;C. D. Santis;R. Sarkar;M. Simon;N. D. Simone;R. Sparvoli;P. Spillantini;Y. I. Stozhkov;V. D. Felice;Y. T. Yurkin. - In: JETP LETTERS. - ISSN 0021-3640. - STAMPA. - 96:(2013), pp. 621-627. [10.1134/s002136401222002x]