  A recent XMM-Newton observation (Zhekov 2014) has revealed diffuse X-ray
emission inside the nebula NGC 2359 around the Wolf-Rayet star WR 7. Taking
advantage of an improved point-source rejection and background subtraction, and
a detailed comparison of optical and X-ray morphology, we have reanalyzed these
X-ray observations. Our analysis reveals diffuse X-ray emission from a blowout
and the presence of emission at energies from 1.0 to 2.0 keV. The X-ray
emission from NGC 2359 can be described by an optically-thin plasma emission
model, but contrary to previous analysis, we find that the chemical abundances
of this plasma are similar to those of the optical nebula, with no magnesium
enhancement, and that two components at temperatures T_1=2x10^6 K and
T_2=5.7x10^7 K are required. The estimated X-ray luminosity in the 0.3 - 2.0
keV energy range is L_X=2x10^33 erg s^-1. The averaged rms electron density of
the X-ray-emitting gas (n_e \lesssim 0.6 cm^-3) reinforces the idea of mixing
of material from the outer nebula into the hot bubble.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena