Abstract

The last few years have seen gamma-ray astronomy maturing and advancing in the field of time-domain astronomy, utilizing source variability on timescales over many orders of magnitudes, from a decade down to a few minutes and shorter, depending on the source. This review focuses on some of the key science issues and conceptual developments concerning the timing characteristics of active galactic nuclei (AGN) at gamma-ray energies. It highlights the relevance of adequate statistical tools and illustrates that the developments in the gamma-ray domain bear the potential to fundamentally deepen our understanding of the nature of the emitting source and the link between accretion dynamics, black hole physics, and jet ejection.

Highlights

  • The last decade has seen tremendous experimental progress in gamma-ray astronomy much beyond simple source detection

  • This paper focuses on some of the key issues and conceptual developments concerning the timing characteristics of active galactic nuclei (AGN) at gamma-ray energies

  • In this case, the jet power that could be tapped for producing radiation is much smaller, roughly by a factor2, so that typically, very high jet powers would be needed to account for the observed very high energy (VHE) emission

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Summary

Introduction

The last decade has seen tremendous experimental progress in gamma-ray astronomy much beyond simple source detection (e.g., see [1,2,3] for a review). In many cases, detailed spectral and timing characterization have become possible allowing one to probe deeply into the nature and physics of these sources. Gamma-ray astronomy has matured and progressed further in the field of time-domain astronomy, utilizing source variability on timescales over many orders of magnitudes, from a decade down to a few minutes and shorter. This paper focuses on some of the key issues and conceptual developments concerning the timing characteristics of AGN (including rapid variability, log-normal flux distributions, power-law noise, and quasi-periodic oscillations) at gamma-ray energies

Rapid Variability at VHE Energies
PDF Shape and Log-Normality
PSD and Power-Law Noise
Quasi-Periodic Variability
A Possible Example
Conclusions

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