Modeling the radio flaring behaviour of 3C273

Details Modeling the radio flaring behaviour of 3C273 Modeling the radio flaring behaviour of 3C273

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..778b&link_type=abstract

MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp

Astronomy and Astrophysics

Astrophysics

Quasars, Time-Varying Systems, Astrophysical Jets, Time Series Analysis, Time Variability, Radio, Microwave, Quasars

Scientific paper

We present a procedure to obtain the observed characteristics of synchrotron outbursts in relativistic jets. We have used a representative radio long-term light curves of 3C273 at 4.8, 8.0, 14.5, 22.0 and 43.0 GHz to derive the spectral and temporal evolution of a typical outburst. The technique consists in an analysis and decomposition of these light curves into a series of twenty identical flares. We fit the same outbursts simultaneously to 3 light curves covering 3 frequencies at radio domain. The development of a flare is a function of time and frequency. We find that the obtained outburst's evolution is in satisfactory qualitative agreement with the expectations of shock models in relativistic jets. The main goal is to obtain the spectral and temporal characteristics of a typical flare. Individual flares differ only by a few parameters when compared with a typical flare. The relevant parameters of three-stage shock models were found in a second approach. Marscher and Gear (1985) identified three stages of the evolution of the shock according to the dominant cooling process of the electrons: the Compton scattering loss phase, the synchrotron radiation loss phase and the adiabatic expansion loss phase.

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