In papers I and II in this series, we presented hydrodynamical simulations ofjet models with parameters representative of the symbiotic system MWC 560.These were simulations of a pulsed, initially underdense jet in a high densityambient medium. Since the pulsed emission of the jet creates internal shocksand since the jet velocity is very high, the jet bow shock and the internalshocks are heated to high temperatures and should therefore emit X-rayradiation. In this paper, we investigate in detail the X-ray properties of thejets in our models. We have focused our study on the total X-ray luminosity andits temporal variability, the resulting spectra and the spatial distribution ofthe emission. Temperature and density maps from our hydrodynamical simulationswith radiative cooling presented in the second paper are used together withemissivities calculated with the atomic database ATOMDB. The jets in our modelsshow extended and variable X-ray emission which can be characterized as a sumof hot and warm components with temperatures that are consistent withobservations of CH Cyg and R Aqr. The X-ray spectra of our model jets showemission line features which correspond to observed features in the spectra ofCH Cyg. The innermost parts of our pulsed jets show iron line emission in the6.4 - 6.7 keV range which may explain such emission from the central source inR Aqr. We conclude that MWC 560 should be detectable with Chandra orXMM-Newton, and such X-ray observations will provide crucial for understandingjets in symbiotic stars.
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