Synthetic Maps of Relativistic Jets The Origin of Bright Features

Details Synthetic Maps of Relativistic Jets The Origin of Bright Features Synthetic Maps of Relativistic Jets The Origin of Bright Features

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20923908s&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #239.08; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

Using hydrodynamic simulations of the flow of relativistic jets, we generate simulated flux maps of their emissivity. We present a method for determining the combination of physical conditions and angle of view that result in an individual radio feature. By analysis of the physical conditions encountered by a given line of sight through the jet, and the effects of relativistic boosting and time-delay, we can understand what combination of events leads to the formation of bright features. We present flux maps of both axially symmetric and fully three dimensional simulated relativistic jets. We show that both angle of view, which determines boost, and time-delay effects have a major impact on the jet's apparent morphology. We display evolutionary sequences, which show the formation of jet structure over time, and demonstrate that some bright features are long-lived relative to the dynamical time scale of the flow. By examining the histories of sample lines of sight, the contributions of both relativistic effects and flow conditions to the formation of bright features are shown. We find that for mildly relativistic jets the radio core arises from Kelvin-Helmholtz instabilities occurring near the axis of flow, while the extended emission is a manifestation of the bow shock. For three dimensional jets, this method allows for a straight forward analysis of radio features arising from a complex flow.

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