We consider the spin evolution of highly magnetized neutron stars in a hypercritical inflow just after their birth in supernovae .
Presence of a strong magnetic field could deform the star and if the symmetry axis of the field is misaligned with that of stellar rotation , the star will be an emitter of gravitational wave .
Here we investigate the possibility of gravitational radiation from such a star when there is a hypercritical inflow onto it .
For doing this we adopt a simplified model of the system in which the star is approximated as a Newtonian spherical polytrope with index N = 1 .
The stellar configuration is slightly deformed away from spherical by the intense magnetic field ; the rotational angular frequency of the star is determined by the balance between the accretion torque and the magnetic dipole radiation .
We take into account the ’ propeller ’ process in which a rotating stellar magnetic field flings away in-falling matter ; the inflow is assumed to be a self-similar advection dominated flow .
An estimation of the characteristic amplitude of the gravitational radiation from such systems is given .
The computation of the signal-to-noise ratio suggests that for the case of an initially rapidly rotating and highly magnetized star ( surface field 10 ^ { 15 } G ) in the Virgo Cluster , its ellipticity would need to be larger than 10 ^ { -5 } in order for the gravitational waves to be observed .