| Abstract : | Polars are a type of magnetic cataclysmic variables (mCVs) which show perfect synchronicity between the spin period of the primary white dwarf (WD) and the orbital period of the binary system. Whereas, Intermediate polars exhibit large asynchronicity between the two periods (>~ 90%). However, there exist a few rare mCVs where the difference between spin and orbital period is much less (<20%), which neither confirms as a true Polar nor an IP. We present the broadband X-ray study of one such unique system — Paloma. Using simultaneous data from XMM-Newton and NuSTAR observatories, covering a 0.3-40 keV energy band, our work highlights the essential properties involving accretion physics and system geometry. We estimate the mass of the WD by measuring the temperature of the strong shock produced by the infalling matter above the WD poles. We notice strong spectral variability over the rotation cycle of the system, indicating the presence of powerful and inhomogeneous intrinsic absorber present near the emission sites. We detect the possibility of photoionised emission from the warm intrinsic absorber, heated up by the emission from the shock. We argue for a tall shock scenario based on the presence of a weak neutral Fe K-alpha line and weak Compton reflection originating from the surface of the WD. Also, we discuss possible explanations behind the significantly strong orbital frequency peak compared to the weak spin frequency peak in the X-ray power spectrum, which is a distinguishing feature of Paloma and not commonplace in traditional IPs. |
