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A recent XMM-Newton observation (Zhekov 2014) has revealed diffuse X-rayemission inside the nebula NGC 2359 around the Wolf-Rayet star WR 7. Takingadvantage of an improved point-source rejection and background subtraction, anda detailed comparison of optical and X-ray morphology, we have reanalyzed theseX-ray observations. Our analysis reveals diffuse X-ray emission from a blowoutand the presence of emission at energies from 1.0 to 2.0 keV. The X-rayemission from NGC 2359 can be described by an optically-thin plasma emissionmodel, but contrary to previous analysis, we find that the chemical abundancesof this plasma are similar to those of the optical nebula, with no magnesiumenhancement, and that two components at temperatures T_1=2x10^6 K andT_2=5.7x10^7 K are required. The estimated X-ray luminosity in the 0.3 - 2.0keV energy range is L_X=2x10^33 erg s^-1. The averaged rms electron density ofthe X-ray-emitting gas (n_e \lesssim 0.6 cm^-3) reinforces the idea of mixingof material from the outer nebula into the hot bubble.

On the diffuse X-ray emission from the Wolf-Rayet Bubble NGC 2359