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We present an X-ray analysis and a model of the nonthermal emission of thepulsar wind nebula (PWN) MSH15-52. We analyzed XMM-Newton data to obtain thespatially resolved spectral parameters around the pulsar PSRB1509-58. Asteepening of the fitted power-law spectra and decrease in the surfacebrightness is observed with increasing distance from the pulsar. In the secondpart of this paper, we introduce a model for the nonthermal emission, based onassuming the ideal magnetohydrodynamic limit. This model is used to constrainthe parameters of the termination shock and the bulk velocity of the leptons inthe PWN. Our model is able to reproduce the spatial variation of the X-rayspectra. The parameter ranges that we found agree well with the parameterestimates found by other authors with different approaches. In the last part ofthis paper, we calculate the inverse Compton emission from our model andcompare it to the emission detected with the H.E.S.S. telescope system. Ourmodel is able to reproduce the flux level observed with H.E.S.S., but not thespectral shape of the observed TeV {\gamma}-ray emission.

Spatially resolved XMM-Newton analysis and a model of the nonthermal emission of MSH 15-52