An anomalous positron abundance in cosmic rays with energies 1.5-100 GeV

被引：1754

作者：

Adriani, O. ^{[2
,3
]}

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

Bazilevskaya, G. A. ^{[6
]}

Bellotti, R. ^{[7
,8
]}

Boezio, M. ^{[9
]}

Bogomolov, E. A. ^{[10
]}

Bonechi, L. ^{[2
,3
]}

Bongi, M. ^{[3
]}

Bonvicini, V. ^{[9
]}

Bottai, S. ^{[3
]}

Bruno, A. ^{[7
,8
]}

Cafagna, F. ^{[8
]}

Campana, D. ^{[5
]}

Carlson, P. ^{[11
]}

Casolino, M. ^{[1
]}

Castellini, G. ^{[12
]}

De Pascale, M. P. ^{[1
,13
]}

De Rosa, G. ^{[5
]}

De Simone, N. ^{[1
,13
]}

Di Felice, V. ^{[1
,13
]}

Galper, A. M. ^{[14
]}

Grishantseva, L. ^{[14
]}

Hofverberg, P. ^{[11
]}

Koldashov, S. V. ^{[14
]}

Krutkov, S. Y. ^{[10
]}

Kvashnin, A. N. ^{[6
]}

Leonov, A. ^{[14
]}

Malvezzi, V. ^{[1
]}

Marcelli, L. ^{[1
]}

Menn, W. ^{[15
]}

Mikhailov, V. V. ^{[14
]}

Mocchiutti, E. ^{[9
]}

Orsi, S. ^{[1
,11
]}

Osteria, G. ^{[5
]}

Papini, P. ^{[3
]}

Pearce, M. ^{[11
,16
]}

Picozza, P. ^{[1
,13
]}

Ricci, M. ^{[17
]}

Ricciarini, S. B. ^{[3
]}

Simon, M. ^{[15
]}

Sparvoli, R. ^{[1
,13
]}

Spillantini, P. ^{[2
,3
]}

Stozhkov, Y. I. ^{[6
]}

Vacchi, A. ^{[9
]}

Vannuccini, E. ^{[3
]}

Vasilyev, G. ^{[10
]}

Voronov, S. A. ^{[14
]}

Yurkin, Y. T. ^{[14
]}

Zampa, G. ^{[9
]}

Zampa, N. ^{[9
]}

机构：

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

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

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

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

[5] Univ Naples Federico II, Sez Naples, I-80126 Naples, Italy

[6] PN Lebedev Phys Inst, RU-119991 Moscow, Russia

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

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

[9] Ist Nazl Fis Nucl, Sez Trieste, I-34012 Trieste, Italy

[10] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia

[11] AlbaNova Univ Ctr, Dept Phys, KTH, SE-10691 Stockholm, Sweden

[12] IFAC, I-50019 Florence, Italy

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

[14] Moscow Engn & Phys Inst, RU-11540 Moscow, Russia

[15] Univ Siegen, D-57068 Siegen, Germany

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

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

来源：

NATURE | 2009年 / 458卷 / 7238期

基金：

瑞典研究理事会; 俄罗斯基础研究基金会;

关键词：

DARK-MATTER; ELECTRON; FRACTION; PARTICLE;

D O I：

10.1038/nature07942

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Antiparticles account for a small fraction of cosmic rays and are known to be produced in interactions between cosmic-ray nuclei and atoms in the interstellar medium(1), which is referred to as a 'secondary source'. Positrons might also originate in objects such as pulsars(2) and microquasars(3) or through dark matter annihilation(4), which would be 'primary sources'. Previous statistically limited measurements(5-7) of the ratio of positron and electron fluxes have been interpreted as evidence for a primary source for the positrons, as has an increase in the total electron+positron flux at energies between 300 and 600 GeV (ref. 8). Here we report a measurement of the positron fraction in the energy range 1.5-100 GeV. We find that the positron fraction increases sharply overmuch of that range, in a way that appears to be completely inconsistent with secondary sources. We therefore conclude that a primary source, be it an astrophysical object or dark matter annihilation, is necessary.

引用

页码：607 / 609

页数：3

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