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The X-ray emission from a simulated massive stellar cluster is investigated.The emission is calculated from a 3D hydrodynamical model which incorporatesthe mechanical feedback from the stellar winds of 3 O-stars embedded in a giantmolecular cloud clump containing 3240 M$_{\odot}$ of molecular material withina 4 pc radius. A simple prescription for the evolution of the stars is used,with the first supernova explosion at t=4.4 Myrs. We find that the presence ofthe GMC clump causes short-lived attenuation effects on the X-ray emission ofthe cluster. However, once most of the material has been ablated away by thewinds the remaining dense clumps do not have a noticable effect on theattenuation compared with the assumed interstellar medium column. We determinethe evolution of the cluster X-ray luminosity, L$_X$, and spectra, and generatesynthetic images. The intrinsic X-ray luminosity drops from nearly 10$^{34}$ergs s$^{-1}$ while the winds are `bottled up', to a near constant value of1.7$\times 10^{32}\rm ergs s^{-1}$ between t=1-4 Myrs. L$_X$ reduces slightlyduring each star's red supergiant stage due to the depressurization of the hotgas. However, L$_X$ increases to $\approx 10^{34}\rm\,ergs s^{-1}$ during eachstar's Wolf-Rayet stage. The X-ray luminosity is enhanced by 2-3 orders ofmagnitude to $\sim 10^{37}\rm ergs s^{-1}$ for at least 4600 yrs after eachsupernova, at which time the blast wave leaves the grid and the X-rayluminosity drops. The X-ray luminosity of our simulation is generallyconsiderably fainter than predicted from spherically-symmetric bubble models,due to the leakage of hot gas material through gaps in the outer shell. Thisprocess reduces the pressure within our simulation and thus the X-ray emission.However, the X-ray luminosities and temperatures which we obtain are comparableto similarly powerful massive young clusters.

Feedback from Winds and Supernovae in Massive Stellar Clusters - II. X-Ray Emission