  We study a white dwarf (WD) - neutron star (NS) reverse evolution that might
lead to the rare explosion of the WD as a type Ia peculiar supernova (peculiar
SN Ia) few months to several years before the core, which is a remnant of a red
supergiant (RSG) star, explodes as a core collapse supernova (CCSN). Using the
evolutionary code \textsc{mesa-binary} we simulate evolution of binary systems
with stars of initial masses of 6-7.5 Mo. The more massive star, the primary,
transfers mass to the secondary star and leaves a CO WD remnant of mass ~ 1 Mo.
The secondary becomes massive enough to end in a CCSN. As the secondary evolves
to the RSG phase it engulfs the WD and the system experience a common envelope
evolution that ends with a WD-core binary system at an orbital separation of
a_f ~ 1-5 Ro. Our simulations show that the core explodes as a CCSN at
t_{CEE-CCSN} ~ 3000 - 10^5 yr after the CEE. The rest of the scenario is
speculative. We assume that if the WD accretes helium-rich gas from the core it
might explode as a SN Ia in the frame of the double detonation scenario for SNe
Ia and peculiar SNe Ia. The peculiar SN Ia explosion might occur at the end of
the CEE evolution or just few years before the CCSN. We predict the very rare
occurrence of a peculiar SN Ia followed within months to years by a CCSN.
