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Constraints on evaporating primordial black holes from the AMS-02 positron data
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abstract
Cosmic-ray (CR) positrons are relatively rare due to their secondary origin and thus sensitive to exotic contributions. Primordial black holes (PBHs) with masses above $\sim 5\times10^{14}\,\mathrm{g}$ can be stable sources of CR positrons due to Hawking radiation. The energies of the evaporated positrons can increase significantly through scattering with the Galactic random magnetic fields during the propagation in the Galaxy, which is a generic feature in diffusive re-acceleration CR propagation models. We show that in well-constrained diffusive re-acceleration models, a significant portion of CR positron flux can enter the energy region of $\mathcal{O}(\text{GeV})$, and can be constrained by the current AMS-02 data. As an example, we show that in the Galprop+Helmod model for CR propagation in the Galaxy and heliosphere, an upper limit of $f_{\text{PBH}}\lesssim2.15\times 10^{-4}$ at PBH mass $2\times 10^{16}$~g can be obtained, which improve the previous constraints from the Voyager CR all-electron data by around an order of magnitude.
Forward citations
Cited by 4 Pith papers
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Revisiting PBH accretion, evaporation and their cosmological consequences
Relativistic accretion onto Kerr primordial black holes gives roughly 4.5x mass growth and fast spin-down, strengthening BBN bounds, lowering the survival mass to ~2.7e14 g, and erasing the high-frequency stochastic g...
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Probing Memory-Burdened Primordial Black Holes with Galactic Sources observed by LHAASO
LHAASO spectra of four Galactic sources are used to set upper limits on the abundance of memory-burdened primordial black holes lighter than 10^9 g.
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Molecular clouds constraints on sub-GeV DM and asteroid-mass PBHs
Molecular-cloud ionization yields competitive constraints on sub-GeV dark matter annihilation/decay and on asteroid-mass primordial black holes, particularly for PBHs above 10^16 g.
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Constraining primordial black holes and primordial curvature power spectrum with extragalactic muon neutrino
Neutrino flux from WIMP annihilation in PBH-seeded UCMHs yields f_PBH ≲ 4×10^{-5} (strongest) and P_R ≲ 10^{-1.65} at k∼3×10^{12} Mpc^{-1}.
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