Kleinnishina effects on optically thin synchrotron and synchrotron self-compton spectrum

Ehud Nakar, Shin'Ichiro Ando, Re'Em Sari

Research output: Contribution to journalArticlepeer-review

Abstract

We present analytic approximations to the optically thin synchrotron and synchrotron self-Compton (SSC) spectra when Klein-Nishina (KN) effects are important and pair production and external radiation fields can be neglected. This theory is useful for analytical treatment of radiation from astrophysical sources, such as gamma-ray bursts (GRBs), active galactic nuclei, and pulsar wind nebula, where KN effects may be important. We consider a source with continuous injection of relativistic electrons with a power-law energy distribution above some typical injection energy. We find that the synchrotron-SSC spectra can be described by a broken power law, and provide analytic estimates for the break frequencies and power-law indices. In general, we show that the dependence of the KN cross section on the energy of the upscattering electron results in a hardening of the energy distribution of fast cooling electrons and therefore in a hardening of the observed synchrotron spectrum. As a result the synchrotron spectrum of fast cooling electrons, below the typical injection energy, can be as hard as F ν ν0, instead of the classical ν-1/2 when KN effects are neglected. The synchrotron energy output can be dominated by electrons with energy above the typical injection energy. We solve self-consistently for the cooling frequency and find that the transition between synchrotron and SSC cooling can result in discontinuous variations of the cooling frequency and the synchrotron and SSC spectra. We demonstrate the application of our results to theory by applying them to prompt and afterglow emission models of GRBs.

Original languageEnglish
Pages (from-to)675-691
Number of pages17
JournalAstrophysical Journal
Volume703
Issue number1
DOIs
StatePublished - 2009

Keywords

  • Galaxies: active
  • Gamma rays: bursts
  • Pulsars: general
  • Radiation mechanisms: non-thermal

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