The astrophysical origin of r -process nuclei remains a long-standing mystery .
Although some astrophysical scenarios show some promise , many uncertainties involved in both the astrophysical conditions and in the nuclear properties far from the \beta -stability have inhibited us from understanding the nature of the r -process .
The purpose of the present paper is to examine the effects of the newly-derived microscopic Hartree-Fock-Bogoliubov ( HFB ) mass formulas on the r -process nucleosynthesis and analyse to what extent a solar-like r -abundance distribution can be obtained .
The r -process calculations with the HFB-2 mass formula are performed , adopting the parametrized model of the prompt explosion from a collapsing O-Ne-Mg core for the physical conditions and compared with the results obtained with the HFB-7 and droplet-type mass formulas .
Due to its weak shell effect at the neutron magic numbers in the neutron-rich region , the microscopic mass formulas ( HFB-2 and HFB-7 ) give rise to a spread of the abundance distribution in the vicinity of the r -process peaks ( A = 130 and 195 ) .
While this effect resolves the large underproduction at A \approx 115 and 140 obtained with droplet-type mass formulas , large deviations compared to the solar pattern are found near the third r -process peak .
It is shown that a solar-like r -process pattern can be obtained if the dynamical timescales of the outgoing mass trajectories are increased by a factor of about 2 - 3 , or if the \beta -decay rates are systematically increased by the same factor .