Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Figure 7

Scenario D: a series of plots for the jet temperature of run4 (run4 parameters in Table 1). This plot shows 2D slices cut along the jet, depicting the temperature on the slice, at a specific time instant. The, faster than previous runs, advance of the jet, through surrounding wind matter, is characterized by an expanding shock front. Said expansion is initially slower, till the jet crosses the simplified accretion disk wind construct. Then, a higher rate of expansion occurs, especially to the sides, as the stellar wind gradient is less pronounced, since we have , where is the jet crossing distance and is the distance to the binary companion star.