MWC 560 (= V694 Mon) is the only known Symbiotic Star system in which the jet axis is practically parallel to the line of sight. Therefore this system is predestinated to study the dynamical evolution and the propagation of stellar jets. Spectroscopic monitoring done by Schmid et al. (2001) showed that the outflow is seen as absorption features in the continuum of the accretion disk and the accreting white dwarf, the emission line spectrum of the accretion disk and the spectrum of the red giant. We present the first numerical simulations of the jet of this particular object using the NIRVANA code (Ziegler & Yorke 1997) in order to reproduce the velocity structures seen in the observational data. This code solves the equations of hydrodynamics and was modified to calculate radiative losses due to non-equilibrium cooling by line-emission (Thiele 2000).
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