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We present an analysis of the XMM-Newton observation of luminous infraredmerging galaxies Arp 302 and a joint re-analysis of its Chandra observation. Inparticular, we focus on the more significant X-ray emitter of the pair, Arp302N. Chandra detects significant soft X-ray emission from the hot gas in thestar-forming region of Arp 302N spreading up to 12 kpc. We estimate thestar-formation rate of Arp 302N to be around 1-2 $M_{\odot}$ yr$^{-1}$ based onthe X-ray luminosity of the star-forming region, similar to previousmeasurements at longer wavelengths. Chandra and XMM-Newton observations showevidence of a Si XIII emission line with 86% confidence. Our best-fit modelinfers a super-solar silicon abundance in the star-forming region, likelyrelated to the past core-collapse supernovae in this galaxy. Similar siliconoverabundance was reported in the circumstellar medium of core-collapsesupernova remnants in our Galaxy.  We also detect narrow Fe K$\alpha$ and Fe K$\beta$ (98.6% confidence)emission lines as part of the AGN emission. Our best-fit spectral model usingMytorus indicates the evidence of a heavily obscured power-law emission with$N_{\rm H}>3\times10^{24}$ cm$^{-2}$ in addition to a weak, unobscuredpower-law emission. The scattering fraction of the unobscured power-lawemission from Compton-thin materials is 0.7%. All these spectral featuressuggest evidence of a Seyfert 2-like AGN in Arp 302N. The X-ray measurement ofits AGN activity is consistent with the previous Spitzer measurement of thesame object.

The Origin of the X-ray Emission from the Non-Starburst Gas-Rich Luminous Infrared Galaxies Arp 302