Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Figure 6

Scenario D: the pressure evolution for the model jet of run4. This plot is similar to the one for the jet density. The patterns are similar to those of the density for the same run. The higher jet’s density dominates the system dynamics, leading to comparatively poorer features around the jet, in relation to other runs where the jet was lighter. The pressure distribution follows the above general pattern. A pressure increase is also seen around the jet base, due to the mass leftover from the disturbed accretion disk wind that used to be there (run4 parameters in Table 1).

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