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X-rays in intermediate polars (IPs) originate in a compact region near thesurface of a magnetic white dwarf (WD) and interact with the complexenvironment surrounding the emission region. Here we report a case study of twoIPs, TV Col and V2731 Oph with selected archival X-ray observations (NuSTAR,Swift, Suzaku, and XMM-Newton). For TV Col, we were successful insimultaneously accounting for the primary X-rays, the secondary X-rays due toCompton scattering and fluorescence, and the effects of local absorbers. Inthis case, we were able to demonstrate that the shock height is small, based onthe high reflection amplitude, and hence the maximum temperature of thepost-shock region can be used to derive the WD mass of 0.735+/-0.015 Msun.Despite the high specific accretion rate required to explain the small shockheight, we do not detect any spin modulation in our NuSTAR data, consistentwith the modest amount of complex absorption seen spectroscopically. We arguethat our results are robust because they are based on the jointtemporal-spectral analysis of broadband X-ray data. The spectrum of V2731 Ophis more highly absorbed. Through our analysis of the Suzaku data, we present aspectral model with nitrogen overabundance without the previously claimed softblackbody that should be further explored. We have been unable to constrainreflection amplitude for V2731 Oph; this and the detection of spin modulationabove 10 keV suggest that it may have a tall shock, hence we only derive alower limit to the mass of its WD (> 0.9 Msun).

Developing the physical understanding of intermediate polars: an X-ray study of TV Col and V2731 Oph