Research
Maps by viewing angle
Maps using relativistic time delay
3D Images
| From the hydrodynamics we know the velocity, the energy density and the mass density. To calculate the synchrotron emissivity we must assume a relationship between these quantities and the distribution of radiating (fast) particles and the magnetic field strength. | |
Jet 1 viewed at 15° and modeled using sound speed. |
Jet 1 viewed at 15° and modeled using pressure. |
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Pressure Model: This model assumes that the radiating particles are the result of
shock-Fermi acceleration of the high energy tail of the particle distribution. The
acceleration takes place in the region where the pressure is highest, so using pressure
to model emissivity gives us a way to trace these particles. Sound Speed Model: In many AGN the most intense emission is not coming from near the high pressure shock front, but rather regions in which the jet material has been shocked. These regions are behind the shock front, where the density is significantly lower than near the bow front. Using sound speed to model the emissivity has the effect of modulating the pressure with the density. The goal of any model for emissivity to to generate maps that reflect the range of structure seen in astrophysical jets. Based on the range of structure revealed by these two models, we believe the sound speed model is more appropriate for mildly relativistic jets, while the pressure model is better suited to highly relativistic jets. |
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Jet 2 viewed at 4° and modeled using sound speed. |
Jet 2 viewed at 4° and modeled using pressure. |