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ASCA Observations of Blazars

Published online by Cambridge University Press:  14 August 2015

T. Takahashi ,
H. Kubo  and
G. Madejski
T. Takahashi
Affiliation:
Institute of Space and Astronautical Science3-1-1 Yoshinodai, Sagamihara, Kanagawa, Japan
H. Kubo
Affiliation:
The Institute of Physical and Chemical Research, 2-1 Hirosawa, Wako, Saitama, 351-01, Japan
G. Madejski
Affiliation:
Laboratory for High Energy Astrophysics, Code 662, NASA GSFC, MD 20771, USA

Extract

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During the last years it has become evident that blazar class of AGN emit a lot of energy in the gamma-ray regime. It is generally thought that the non-thermal emission from blazars, observed from radio to GeV/TeV 7-rays, is radiation of very energetic particles via both synchrotron and Compton processes. This underlines the importance of high-energy emission for models of the blazar class of active galactic nuclei. Most of the gamma-bright AGN are variable, and flares with time scales as short as a day have been observed. This suggests that the site of gamma-ray emission is very compact and situated in a fluid which moves relativistically at a small angle towards the observer. It is generally assumed that the emission originates from the jet of these objects.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 2: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part B), 1997 , 1998 , pp. 812 - 815
Copyright
Copyright © Kluwer 1998

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