Kavli Affiliate: Claudio Ricci
| First 5 Authors: Sibasish Laha, Claudio Ricci, John C. Mather, Ehud Behar, Luigi C. Gallo
| Summary:
Active galactic nuclei (AGN) are powerful sources of panchromatic radiation.
All AGN emit in X-rays, contributing around $sim 5-10%$ of the AGN bolometric
luminosity. The X-ray emitting region, popularly known as the corona, is
geometrically and radiatively compact with a size typically $lesssim 10 ,
R_{rm G}$ (gravitational radii). The rapid and extreme variability in X-rays
also suggest that the corona must be a dynamic structure. Decades of X-ray
studies have shed much light on the topic, but the nature and origin of AGN
corona are still not clearly understood. This is mostly due to the complexities
involved in several physical processes at play in the high-gravity,
high-density and high-temperature region in the vicinity of the supermassive
black hole (SMBH). It is still not clear how exactly the corona is
energetically and physically sustained near a SMBH. The ubiquity of coronal
emission in AGN points to their fundamental role in black hole accretion
processes. In this review we discuss the X-ray observational properties of
corona in radio quiet AGN.
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