2025/02/24 by Alexandre Arbey, Marco Calzà, Arbey, Alexandre +3 · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Physics - Phenomenology (hep-ph) #High Energy Physics - Theory (hep-th)
paper · pdf · doi:10.48550/arxiv.2502.17240
openalex publication_date 2025/02/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The calculation of gray-body factors is essential for understanding Hawking radiation and black hole thermodynamics. While the formalism developed by Chandrasekhar is effective for static black holes, it faces significant challenges in Kerr spacetimes, particularly in the superradiant regime, where a specific choice of coordinates introduces numerical inaccuracies. To address these limitations, an alternative method based on re-scaling radial coordinates and employing Frobenius-like expansions has been investigated. We compare the gray-body factors obtained for a near-maximally rotating black hole using both methods and find that the Chandrasekhar formalism systematically overestimates the values in the superradiant regime compared to well-established analytical results. Specifically, for a spin parameter of a_* = 0.999, the Chandrasekhar method yields values approximately twice as large as the correct result. Since this approach has been implemented in BlackHawk, we assess the impact of these discrepancies on constraints derived from gamma-ray observations of highly spinning primordial black holes.