  The role and implication of binding energy through the accretion-induced
collapse (AIC) of accreting white dwarfs (WDs) for the production of
millisecond pulsars (MSPs) are investigated. I examine the binding energy model
due to the dynamical process in close binary systems and investigating the
possible mass of the companion sufficient to induce their orbital parameters.
The deterministic nature of this interaction has a strong sensitivity to the
equation of state of the binary systems (where the compactness of a neutron
star is proportional to the amount of binding energy) associated with their
initial conditions. This behavior will mimic the commonly assumed mass and
amount of accreted matter under the instantaneous mass loss ($\Delta M \sim
0.18M_{\odot}$). As a result, this will indicate an increase in the MSP's
gravitational mass due to angular momentum losses. The outcome of such a system
will then be a circular binary MSP in which the companion is a low-mass WD,
thus distinguishing the binary formation scenarios. In addition, the results of
this work could provide constraints on the expected mass and binding energy of
a neutron star based on the accretion rate
