We present analyses of archival X-ray data obtained from the XMM-Newton and Suzaku satellites of an intermediate polar RXJ 1712-2414. The X-ray
variations occur at the spin and synodic periods, supporting the view that this is a disc-overflow accreting system. The X-ray spectrum is strongly
absorbed by a dense material with an average equivalent hydrogen column density of ~5×1022 cm−2 , which partially covers ~46 % of the X-ray source. Using the Suzaku spectra in 0.3-50 keV energy range, which is well explained by two temperatures collisional equilibrium plasma emission models with its reflection from the cold matter, the post-shock temperature is estimated to be 26 keV. A soft X-ray excess is seen in the X-ray spectrum of RXJ 1712-2414 and well modeled by the black-body with an average temperature of 98 eV. The spin phase resolved spectroscopy of RXJ 1712-2414 in 0.3-10.0 keV energy range shows that the spectral parameters are phase dependent. The spin phase dependent softness ratio indicate that coverage of accretion curtains is variable. A strong fluorescent Fe Kalpha emission line is also detected with the large values of reflection component and equivalent width,
indicating that this is due to the reflection from the WD surface. The central energy of Fe Kalpha appears to be red-shifted and found to be modulated with the WD rotation, where modulations are minimum around the spin
minimum, indicating that the red-shifted line is originated from pre-shock accreting material via fluorescence.