A detailed analysis of X-ray data obtained with ROSAT , ASCA , XMM - Newton and the Rossi X - ray Timing Explorer ( RXTE ) for the asynchronous polar V1432 Aquilae is presented .
An analysis of Stokes polarimetry data obtained from the South African Astronomical Observatory ( SAAO ) is also presented .
Power spectra from long-baseline ROSAT data show a spin period of 12150 s along with several frequency components related to the source .
However , the second harmonic of the spin period dominates the power spectrum in the XMM - Newton data .
For the optical circular polarization , the dominant period corresponds to half the spin period ( or its first harmonic ) .
The ROSAT data can be explained as due to accretion onto two hot spots that are not anti-podal .
The variations seen in the optical polarization and the ASCA and XMM - Newton X-ray data suggest the presence of at least three accretion foot prints on the surface of the white dwarf .
Two spectral models , a multi-temperature plasma model and a photo-ionized plasma model , are used to understand the spectral properties of V1432 Aql .
The data from the RXTE Proportional Counter Array ( PCA ) with its extended high energy response are used to constrain the white dwarf mass to 1.2 \pm 0.1 M _ { \odot } using a multi-temperature plasma model .
The data from the European Photon Imaging Camera ( EPIC ) on-board XMM - Newton are well fitted by both models .
A strong soft X-ray excess ( < 0.8 keV ) is well modeled by a blackbody component having a temperature of 80–90 eV .
The plasma emission lines seen at 6.7 and 7.0 keV are well fitted using the multi-temperature plasma model .
However , the fluorescent line at 6.4 keV from cold Fe requires an additional Gaussian component .
The multi-temperature plasma model requires two absorbers : one that covers the source homogeneously and another partial absorber covering \sim 65 % of the source .
The photo-ionized plasma model , with a range of column densities for the Fe ions , gives a slightly better overall fit and fits all emission line features .
The intensity and spectral modulations due to the rotation of the white dwarf at a period of 12150 s require varying absorber densities and a varying covering fraction of the absorber for the multi-temperature plasma model .
The presence of a strong blackbody component , a rotation period of 12150 s , modulation of the Fe fluorescence line flux with 12150 s period , and a very hard X-ray component suggest that V1432 Aql is an unusual polar with X-ray spectral properties similar to that of a soft intermediate polar .