Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...430..550s&link_type=abstract
The Astrophysical Journal, vol. 430, no. 2, pt. 1, p. 550-567
Astronomy and Astrophysics
Astronomy
24
Absorption Spectra, Compton Effect, Electron Sources, Galactic Nuclei, Radio Emission, Radio Spectra, Relativistic Electron Beams, Synchrotron Radiation, Astronomical Models, Brightness Temperature, Computerized Simulation, Cosmology, Radiative Transfer, Radio Sources (Astronomy), Spectrum Analysis
Scientific paper
We present a model of the radio emission from synchrotron self-absorbed sources, including the effects of induced Compton scattering by the relativistic electrons in the source. Order of magnitude estimates show that stimulated scattering becomes the dominant absorption process when (kTB/me c2)TauT greater than or approximately 1.0. Numerical simulations demonstrate that relativistic induced Compton scattering limits the brightness temperature of a self-absorbed synchroton sources to TB less than or approximately 2 x 1011 nu-1/p + 3 zero, 9 gammap + 2/p + 5 min K, where gammamin is the low-energy cutoff to the relativistic electron distribution with a power-law index of p. It can also significantly flatten the radio spectrum. The radio spectrum of the core of 3C 279 is well matched by a model in which stimulated scattering is important, and the additional constraint TB less than 2 x 1011K may be important to the interpretation of the broadband spectra in variable extragalactic compact radio sources. Stimulated scattering reduces the amplitude of the radio frequency variability relative to the X-ray variability, an effect which can be detected by multiwavelength variability studies. Data for a sample of resolved compact radio cores indicate that it is inconsistent to neglect induced Compton scattering when inferring the physical parameters of the sources. The necessary generalizations to the standard synchrotron self-Compton theory are p resented.
Krolik Julian H.
Sincell Mark W.
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