  A White Dwarf (WD) star and a main-sequence companion may interact through
their different stellar evolution stages. This sort of binary population has
historically helped us improve our understanding of binary formation and
evolution scenarios. The data set used for the analysis consists of 115
well-measured WD masses obtained by the Sloan Digital Sky Survey (SDSS). A
substantial fraction of these systems could potentially evolve and reach the
Chandrasekhar limit, and then undergo an Accretion-Induced Collapse (AIC) to
produce millisecond pulsars (MSPs). I focus my attention mainly on the massive
WDs (M_WD > 1M_sun), that are able to grow further by mass-transfer phase in
stellar binary systems to reach the Chandrasekhar mass. A mean value of M ~
1.15 +/- 0.2M_sun is being derived. In the framework of the AIC process, such
systems are considered to be good candidates for the production of MSPs. The
implications of the results presented here to our understanding of binary MSPs
evolution are discussed. As a by-product of my work, I present an updated
distribution of all known pulsars in Galactic coordinates pattern. Keywords:
Stars; Neutron stars; White dwarfs; X-ray binaries; Fundamental parameters.
