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In this article, we will analytically explore how a recollimation shock can explain stationary X-ray emission from jets. Based on the observational evidence for multi-layered jets, we assume that the innermost component of the flow is a stellar wind, which is collimated by the disk wind, which feeds the outer layers of the flow. Collimation shocks of this kind have not been treated in detail in the literature, while X-ray emission due to a moving shocks has been studied by several authors \citep[see, e.g.\ the analytical work and numerical simulations by][]{http://adsabs.harvard.edu/abs/2002ApJ...576L.149R,http://adsabs.harvard.edu/abs/2007A&A...462..645B,http://adsabs.harvard.edu/abs/2010A&A...517A..68B}.  \citet{2011ApJ...737...54B} numerically simulated stationary X-ray shocks. To do so, they impose a rigid nozzle with a radius of a few hundred AU and inject a flow of plasma with a flat velocity profile along the jet axis. They find that a diamond diamond-shaped  shock forms at a hight roughly twice the radius of the nozzle, where the nozzle with a  temprature are high enough to explain the X-ray emission ffrom from  HH~154. In contrast to that work, we do not impose rigid boundaries that collimate the flow, but instead prescribe an external presure profile and then calculate the position of the boundary between the inner wind and the external medium. Also, the setup of \citet{2011ApJ...737...54B} is well-suited to study regions at larger distance from the star, but in this article we concentate on the inner few AU, region,  where the outflow is not yet parallel to the jet axis. Instead, axis and stellar and disk outflow have different velocities. Thus,  we start with a spherical flow from the stellar surface and explain how a shock can be caused by the recollimation of the inner jet stellar outflow  due to presure from  the shape of the boundary between stellar winds and outer  disk winds winds. We use a model  similar to the work of \citet{2012MNRAS.422.2282K} for relativistic jets.