Observational Appearance of Optically Thin, Relativistic Winds

Details Observational Appearance of Optically Thin, Relativistic Winds Observational Appearance of Optically Thin, Relativistic Winds

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..402..396s&link_type=abstract

Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies ASP Conference Series, Vol. 402, proceedings o

Astronomy and Astrophysics

Astrophysics

Scientific paper

Synchrotron radiation is often observed in the objects that are believed to harbor the black hole and the accretion disk at the galaxy center, such as active galactic nuclei (AGN) and quasars. For example, it is believed that the jets and the radio-emitting lobes are strong synchrotron-emission sources. Moreover, the broad-band spectrum energy distribution (SED) of the objects belongs to the blazar class of AGN and shows two components with the lower-energy one attributed to synchrotron radiation by relativistic electrons. Hence, synchrotron radiation is an important radiation process for those objects. Thus, we assume that the plasma gas with magnetic fields blows off as relativistic, spherically symmetric, optical thin winds from the center of the object like AGN, and we calculate the spectrum of the hybrid thermal-nonthermal synchrotron emissions.

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