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Open AccessFeature PaperArticle

Sub-Hour X-Ray Variability of High-Energy Peaked BL Lacertae Objects

Astrophysical Observatory, Ilia State University, Colokashvili Av. 3/5, Tbilisi 0162, Georgia
INAF, Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, Italy
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1107, USA
Galaxies 2018, 6(1), 37;
Received: 2 January 2018 / Revised: 26 February 2018 / Accepted: 7 March 2018 / Published: 15 March 2018
(This article belongs to the Special Issue Microvariability of Blazars)
The study of multi-wavelength flux variability in BL Lacertae objects is very important to discern unstable processes and emission mechanisms underlying their extreme observational features. While the innermost regions of these objects are not accessible from direct observations, we may draw conclusions about their internal structure via the detection of flux variations on various timescales, based on the light-travel argument. In this paper, we review the sub-hour X-ray variability in high-energy peaked BL Lacertae sources (HBLs) that are bright at X-rays and provide us with an effective tool to study the details related to the physics of the emitting particles. The X-ray emission of these sources is widely accepted to be a synchrotron radiation from the highest-energy electrons, and the complex spectral variability observed in this band reflects the injection and radiative evolution of freshly-accelerated particles. The detection of sub-hour X-ray flux variability is very important since it can be related to the small-scale jet turbulent structures or triggered by unstable processes occurring in the vicinity of a central supermassive black hole. We summarize the fastest X-ray variability instances detected in bright HBLs and discuss their physical implications. View Full-Text
Keywords: BL Lacertae objects: individual: Mrk 421 BL Lacertae objects: individual: Mrk 421
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Kapanadze, B. Sub-Hour X-Ray Variability of High-Energy Peaked BL Lacertae Objects. Galaxies 2018, 6, 37.

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