  Numerous studies on hydrodynamics of the Keplerian as well as the
sub-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 or
an NS) has a finite surface, its rapid rotation, the stellar magnetic field
could cause deformation of the spherical symmetry. Earlier studies for
Keplerian disc showed that a deviation from the spherical symmetry of the
compact object could affect the observed light curve and spectra at high
frequencies. Here, we have explored the effect of the non-spherical nature of a
compact object on the hydrodynamics of an optically thin, geometrically thick
sub-Keplerian advective flow. We find that due to non-spherical shape of the
central accretor, there is a possibility to trigger Rankine-Hugoniot shock in
the sub-Keplerian advective flow close to the accretor without considering any
general relativistic effect or presence of the hard surface of the star. Our
results are more relevant for accretion onto WD as hardly any general
relativistic effect will come in the picture. We propose that some
observational features e.g., high significance of fitting the spectra with
multi-temperature plasma models rather than single temperature models, and
variable efficiency of X-ray emission (X-ray luminosity in comparison with
optical and UV luminosity of the disk) in nonmagnetic cataclysmic variables can
be explained by the presence of a shock in the sub-Keplerian advective flow.
