  The evolution of a star of initial mass 10 $M_{\odot}$, and metallicity $Z =
0.02$ in a Close Binary System (CBS) is followed from its main sequence until
an ONe degenerate remnant forms. Restrictions have been made on the
characteristics of the companion as well as on the initial orbital parameters
in order to avoid the occurrence of reversal mass transfer before carbon is
ignited in the core. The system undergoes three mass loss episodes. The first
and second ones are a consequence of a case B Roche lobe overflow. During the
third mass loss episode stellar winds may play a role comparable to, or even
more important than Roche lobe overflow. In this paper, we extend the
previously existing calculations of stars of intermediate mass belonging to
close binary systems by following carefully the carbon burning phase of the
primary component. We also propose different possible outcomes for our scenario
and discuss the relevance of our findings. In particular, our main result is
that the resulting white dwarf component of mass $1.1 M_\odot$ more likely has
a core composed of oxygen and neon, surrounded by a mantle of carbon-oxygen
rich material. The average abundances of the oxygen-neon rich core are $X({\rm
O}^{16})=0.55$, $X({\rm Ne}^{20})=0.28$, $X({\rm Na}^{23})=0.06$ and $X({\rm
Mg}^{24})=0.05$. This result has important consequences for the Accretion
Induced Collapse scenario. The average abundances of the carbon-oxygen rich
mantle are $X({\rm O}^{16})=0.55$, and $X({\rm C}^{12})=0.43$. The existence of
this mantle could also play a significant role in our understanding of
cataclysmic variables.
