Inverse Compton angular kernels and Klein–Nishina regime
Research context
research method · conditional · As of 2026-10-10
Inverse Compton energy gain depends on incident angle and the photon energy in the electron rest frame.
Key knowledge
Inverse Compton energy gain depends on incident angle and the photon energy in the electron rest frame. The Thomson limit fails as that energy approaches the electron rest energy; a Klein–Nishina kernel changes both scattering probability and loss spectrum.
Values and equations
ε'=γ ε(1-β cos θ_i); ε'_f/ε'_i=[1+(ε'_i/(m_e c^2))(1-cos θ')]^-1
- ε,ε'_i,ε'_f
- Lab incident and rest-frame photon energies J
- γ
- Electron Lorentz factor 1
- β
- Electron speed divided by c 1
- θ_i
- Lab incident angle to electron velocity rad
- θ'
- Rest-frame scattering angle rad
- m_e
- Electron mass kg
- c
- Speed of light m s^-1
Conditions and scope
- The existing isotropic Thomson-loss record is a conditional limit, not an anisotropic high-energy kernel.
- Use target-photon angular/spectral distribution, electron population and relativistic geometry before fitting spectra.
Sources · 2
References
Sources retain their recorded scope. A source link alone does not establish verification of every statement.
Evidence and review
High energy astrophysics: Compton scattering: Slides 10–18: Klein–Nishina differential cross section and incident-angle dependence (selected source body inspected). High energy astrophysics: inverse Compton radiation: Thomson scattering, inverse Compton spectra and synchrotron-self-Compton (selected source body inspected).
2026-10-10 · Bounded source check of the recorded statement and conditions. This does not certify a unique physical model, reproduce the cited study or replace independent branch review.
Entry details
Permanent link to this entry ↗- Record identity
- research-earth-compton-angular
- Revision
- research.1
- Structured reference record
- Postgraduate & research reference