Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Figure 3

Scenario C: a series of slices representing the time evolution of temperature, as in scenario A of [13], but now assuming increased precession rate (see text). The temperature image depicts 2D slices cut along the jet, at a specific time instant. The precessing jet can be seen (d,e) to sweep across a larger (compared to scenario A [13]) portion of the surrounding wind volume, piling up additional matter around its head and sides (see run3 parameters in Table 1). The expansion rate is lower in the accretion disk wind region and increases in the stellar wind region, but afterwards it stays relatively constant, as the density gradient of the wind (visible in the images) is not too large along the jet path.