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Black hole X-ray spectra: notes on the relativistic calculations

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arxiv 2408.12262 v1 pith:5NQZT7JR submitted 2024-08-22 astro-ph.HE gr-qc

Cosimo Bambi This is my paper
classification astro-ph.HEgr-qc
keywords blackcalculationscomponentnotesdiskholerelativisticspectra
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This is a collection of notes to calculate electromagnetic spectra of geometrically thin and optically thick accretion disks around black holes. The presentation is intentionally pedagogical and most calculations are reported step by step. In the disk-corona model, the spectrum of a source has three components: a thermal component from the disk, a Comptonized component from the corona, and a reflection component from the disk. These notes review only the relativistic calculations. The formulas presented here are valid for stationary, axisymmetric, asymptotically-flat, circular spacetimes, so they can be potentially used for a large class of black hole solutions.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Iron K$\alpha$ signatures from accretion disks around fermionic dark matter cores

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    Iron K-alpha line profiles computed in the Ruffini-Argüelles-Rueda fermionic dark matter metric show that the most compact non-rotating cores mimic high-spin Kerr lines and can reproduce MCG-06-30-15.

  2. Testing non-circular black hole spacetime with X-ray reflection

    gr-qc 2026-02 conditional novelty 6.0 of 10

    X-ray reflection data for EXO 1846–031 cannot distinguish the non-circular deformation parameter ℓ_NP from zero, remaining consistent with the Kerr hypothesis.

  3. Assessing systematic uncertainties from spectral re-analysis of Cyg X-1 with different coronal geometries

    astro-ph.HE 2025-12 conditional novelty 6.0 of 10

    Re-analysis of Cyg X-1 NuSTAR/Suzaku spectra shows that the assumed coronal geometry shifts inferred spin (a* ≈ 0.73–0.99) and inclination (≈27°–70°), with a disk-like corona yielding i ≈ 30° and density ≈ 1e20 cm^-3.

  4. Physics and Astrophysics of Black Holes with eXTP

    astro-ph.HE 2026-07 accept novelty 2.0 of 10

    eXTP’s larger effective area and simultaneous polarimetry will tighten black-hole spin and Kerr-deviation constraints relative to NICER for the same exposure.

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