Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Figure 5

Scenario D: a series of snapshots depicting the density evolution (logarithmic plots) for the run4. Here we can see 3D plots of the jet proton density in space, at specific time instants of the simulation run. This time the jet is quite much heavier than both surrounding winds, leading to a decreased jet crossing time of the model space. The jet mass flow rate now rests closer to the estimates for SS433. The jet breaks through the accretion disk wind construct and soon crosses the stellar wind at a rapid pace (run4 parameters in Table 1, snapshot intervals of 50/count).

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