  We present results of X-ray spectroscopy for TWA 5, a member of the young TW
Hydrae association, observed with XMM-Newton. TWA~5 is a multiple system which
shows Halpha emission, a signature typical of classical T Tauri stars, but no
infrared excess. From the analysis of the RGS and EPIC spectra, we have derived
the emission measure distribution vs. temperature of the X-ray emitting plasma,
its abundances, and the electron density. The characteristic temperature and
density of the plasma suggest a corona similar to that of weak-line T Tauri
stars and active late-type main sequence stars. TWA 5 also shows a low iron
abundance (~0.1 times the solar photospheric one) and a pattern of increasing
abundances for elements with increasing first ionization potential reminiscent
of the inverse FIP effect observed in highly active stars. The especially high
ratio Ne/Fe~10 is similar to that of the classical T Tauri star TW Hya, where
the accreting material has been held responsible for the X-ray emission. We
discuss the possible role of an accretion process in this scenario. Since all T
Tauri stars in the TW Hydrae association studied so far have very high Ne/Fe
ratios, we also propose that environmental conditions may cause this effect.
