2020/07/31 by Hyungjin Kim · 55 citations
Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Black hole (networking) #Cosmology and Gravitation Theories #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Hawking radiation #Micro black hole #Physics #Primordial black hole #Spin-flip #astro-ph.CO #astro-ph.GA #hep-ph
paper · pdf · doi:10.1093/mnras/stab1222
published in Monthly Notices of the Royal Astronomical Society 504(4), 5475-5484 (Oxford University Press) · 10 pages, 5 figures; discussion extended, minor typos/numerical error corrected, conclusion unchanged, matches the version accepted for publication in MNRAS
openalex created_date 2020/07/23 · openalex publication_date 2021/04/27 · arxiv created 2021/05/06 · arxiv updated 2021/05/12 · openalex updated_date 2026/08/06
ABSTRACT Primordial black holes are a viable dark matter candidate. They decay via Hawking evaporation. Energetic particles from the Hawking radiation interact with interstellar gas, depositing their energy as heat and ionization. For a sufficiently high Hawking temperature, fast electrons produced by black holes deposit a substantial fraction of energy as heat through the Coulomb interaction. Using the dwarf galaxy Leo T, we place an upper bound on the fraction of primordial black hole dark matter. For M \lt 5 × 10-17 M_\odot, our bound is competitive with or stronger than other bounds.