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Numerous studies on hydrodynamics of the Keplerian as well as thesub-Keplerian accretion disc around a compact object (e.g., white dwarf (WD),neutron star (NS), or a black hole (BH)) attempted to explain the observed UV,soft and hard X-ray spectra. Although, when the compact object (e.g., a WD oran NS) has a finite surface, its rapid rotation, the stellar magnetic fieldcould cause deformation of the spherical symmetry. Earlier studies forKeplerian disc showed that a deviation from the spherical symmetry of thecompact object could affect the observed light curve and spectra at highfrequencies. Here, we have explored the effect of the non-spherical nature of acompact object on the hydrodynamics of an optically thin, geometrically thicksub-Keplerian advective flow. We find that due to non-spherical shape of thecentral accretor, there is a possibility to trigger Rankine-Hugoniot shock inthe sub-Keplerian advective flow close to the accretor without considering anygeneral relativistic effect or presence of the hard surface of the star. Ourresults are more relevant for accretion onto WD as hardly any generalrelativistic effect will come in the picture. We propose that someobservational features e.g., high significance of fitting the spectra withmulti-temperature plasma models rather than single temperature models, andvariable efficiency of X-ray emission (X-ray luminosity in comparison withoptical and UV luminosity of the disk) in nonmagnetic cataclysmic variables canbe explained by the presence of a shock in the sub-Keplerian advective flow.

Advective accretion onto a non-spherical accretor in white dwarf and neutron star binaries: a new scenario of shock formation