  We present an analysis of the XMM-Newton observation of luminous infrared
merging galaxies Arp 302 and a joint re-analysis of its Chandra observation. In
particular, we focus on the more significant X-ray emitter of the pair, Arp
302N. Chandra detects significant soft X-ray emission from the hot gas in the
star-forming region of Arp 302N spreading up to 12 kpc. We estimate the
star-formation rate of Arp 302N to be around 1-2 $M_{\odot}$ yr$^{-1}$ based on
the X-ray luminosity of the star-forming region, similar to previous
measurements at longer wavelengths. Chandra and XMM-Newton observations show
evidence of a Si XIII emission line with 86% confidence. Our best-fit model
infers a super-solar silicon abundance in the star-forming region, likely
related to the past core-collapse supernovae in this galaxy. Similar silicon
overabundance was reported in the circumstellar medium of core-collapse
supernova 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 using
Mytorus indicates the evidence of a heavily obscured power-law emission with
$N_{\rm H}>3\times10^{24}$ cm$^{-2}$ in addition to a weak, unobscured
power-law emission. The scattering fraction of the unobscured power-law
emission from Compton-thin materials is 0.7%. All these spectral features
suggest evidence of a Seyfert 2-like AGN in Arp 302N. The X-ray measurement of
its AGN activity is consistent with the previous Spitzer measurement of the
same object.
