A robust excess in the cosmic-ray antiproton spectrum: Implications for annihilating dark matter

被引：114

作者：

Cholis, Ilias ^{[1
]}

Linden, Tim ^{[2
,3
]}

Hooper, Dan ^{[4
,5
]}

机构：

[1] Oakland Univ, Dept Phys, Rochester, MI 48309 USA

[2] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, Columbus, OH 43210 USA

[3] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[4] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA

[5] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

来源：

PHYSICAL REVIEW D | 2019年 / 99卷 / 10期

关键词：

P-P; INCLUSIVE PRODUCTION; PARTICLE-PRODUCTION; PROPAGATION; COLLISIONS; MOMENTUM;

D O I：

10.1103/PhysRevD.99.103026

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

An excess of similar to 10-20 GeV cosmic-ray antiprotons has been identified in the spectrum reported by the AMS-02 Collaboration. The systematic uncertainties associated with this signal, however, have made it difficult to interpret these results. In this paper, we revisit the uncertainties associated with the time, charge and energy-dependent effects of solar modulation, the antiproton production cross section, and interstellar cosmic-ray propagation. After accounting for these uncertainties, we confirm the presence of a 4.7 sigma antiproton excess, consistent with that arising from a m(chi) approximate to 64-88 GeV dark matter particle annihilating to b (b) over bar with a cross section of sigma v similar or equal to (0.8-5.2) x 10(-26) cm(3)/s. If we allow for the stochastic acceleration of secondary antiprotons in supernova remnants, the data continue to favor a similar range of dark matter models (m(chi) approximate to 46-94 GeV, sigma v approximate to (0.7-3.8) x 10(-26) cm(3)/s) with a significance of 3.3 sigma. The same range of dark matter models that are favored to explain the antiproton excess can also accommodate the excess of GeV-scale gamma rays observed from the Galactic center.

引用

页数：12

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