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

被引：100

作者：

Adriani, O. ^{[1
,2
]}

Bazilevskaya, G. A. ^{[3
]}

Barbarino, G. C. ^{[4
,5
]}

Bellotti, R. ^{[6
,7
]}

Boezio, M. ^{[8
]}

Bogomolov, E. A. ^{[9
]}

Bonvicini, V. ^{[8
]}

Bongi, M. ^{[2
]}

Bonechi, L. ^{[1
,2
]}

Borisov, S. V. ^{[10
,11
,12
]}

Bottai, S. ^{[2
]}

Bruno, A. ^{[6
,7
]}

Vacchi, A. ^{[8
]}

Vannuccini, E. ^{[2
]}

Vasilyev, G. I. ^{[9
]}

Voronov, S. A. ^{[12
]}

Wu, J. ^{[13
,14
]}

Galper, A. M. ^{[12
]}

Grishantseva, L. A. ^{[12
]}

Danilchenko, I. A. ^{[12
]}

Gillard, W. ^{[13
,14
]}

Jerse, G. ^{[8
,16
]}

Zampa, G. ^{[8
]}

Zampa, N. ^{[8
]}

Zverev, V. G. ^{[12
]}

Casolino, M. ^{[10
,19
]}

Campana, D. ^{[5
]}

Carbone, R. ^{[5
,11
]}

Karelin, A. V. ^{[12
]}

Carlson, P. ^{[13
,14
]}

Castellini, G. ^{[15
]}

Cafagna, F. ^{[7
]}

Kvashnin, A. N. ^{[3
]}

Koldashov, S. V. ^{[12
]}

Koldobskiy, S. A. ^{[12
]}

Krutkov, S. Y. ^{[9
]}

Consiglio, L. ^{[5
]}

Leonov, A. A. ^{[12
]}

Mayorov, A. G. ^{[12
]}

Malakhov, V. V. ^{[12
]}

Malvezzi, W. ^{[10
]}

Marcelli, L.

Menn, W. ^{[17
]}

Mikhailov, V. V. ^{[12
]}

Mocchiutti, E. ^{[8
]}

Monaco, A. ^{[6
,7
]}

Mori, N. ^{[1
,2
]}

Nikonov, N. N. ^{[9
,10
,11
]}

Osteria, G. ^{[5
]}

Palma, F. ^{[9
,10
]}

机构：

[1] Univ Florence, Dept Phys, I-50019 Florence, Italy

[2] Ist Nazl Fis Nucl, Sez Florence, I-50019 Florence, Italy

[3] Russian Acad Sci, Lebedev Phys Inst, Moscow 119991, Russia

[4] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy

[5] Ist Nazl Fis Nucl, Sez Naples, I-80126 Naples, Italy

[6] Univ Bari, Dept Phys, I-70126 Bari, Italy

[7] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[8] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy

[9] Russian Acad Sci, Ioffe Phys Tech Inst, St Petersburg 194021, Russia

[10] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, I-00133 Rome, Italy

[11] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy

[12] Natl Res Nucl Univ MEPhI, Moscow 115409, Russia

[13] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden

[14] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[15] IFAC, I-50019 Florence, Italy

[16] Univ Trieste, Dept Phys, I-34147 Trieste, Italy

[17] Univ Siegen, Dept Phys, D-57068 Siegen, Germany

[18] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy

[19] RIKEN, Adv Sci Inst, Wako, Saitama, Japan

来源：

JETP LETTERS | 2013年 / 96卷 / 10期

关键词：

MATTER;

D O I：

10.1134/S002136401222002X

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

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.

引用

页码：621 / 627

页数：7

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