https://doi.org/10.1140/epjc/s10052-024-12773-y
Regular Article - Theoretical Physics
Constraining primordial black holes as dark matter using AMS-02 data
1
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
2
School of Astronomy and Space Science, University of Science and Technology of China, 230026, Hefei, Anhui, China
3
School of Physics and Physical Engineering, Qufu Normal University, 273165, Qufu, Shandong, China
4
Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing University-Purple Mountain Observatory, 210093, Nanjing, China
b
xupan@pmo.ac.cn
d
zulei@pmo.ac.cn
e
ypyang@qfnu.edu.cn
f
fenglei@pmo.ac.cn
Received:
2
February
2024
Accepted:
7
April
2024
Published online:
11
June
2024
Primordial black holes (PBHs) are the plausible candidates for the cosmological dark matter. Theoretically, PBHs with masses 
in the range of 
can emit sub-GeV electrons and positrons through Hawking radiation. Some of these particles could undergo diffusive reacceleration during propagation in the Milky Way, potentially reaching energies up to the GeV level observed by AMS-02. In this work, we utilize AMS-02 data to constrain the PBH abundance 
by employing the reacceleration mechanism. Under the assumption of a monochromatic PBH mass distribution, our findings reveal that the limit is stricter than that derived from Voyager 1 data. This difference is particularly pronounced when 
, exceeding an order of magnitude. The constraints are even more robust in a more realistic scenario involving a log-normal mass distribution of PBHs. Moreover, we explore the impact of varying propagation parameters and solar modulation potential within reasonable ranges, and find that such variations have minimal effects on the final results.
The original online version of this article was revised: Xu Pan should have been denoted as a co-corresponding author.
An erratum to this article is available online at https://doi.org/10.1140/epjc/s10052-024-13007-x.
Copyright comment corrected publication 2024
© The Author(s) 2024. corrected publication 2024
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