  The abrupt and permanent changes of photospheric magnetic field in the
localized regions of active regions during solar flares called magnetic
imprints (MIs), have been observed for the past nearly three decades. The well
known "coronal implosion" model is assumed to explain such flare associated
changes but the complete physical understanding is still missing and debatable.
In this study, we made a systematic analysis of flare-related changes of
photospheric magnetic field during 21 flares (14 eruptive and 7 non-eruptive)
using the high-cadence (\texttt{135s}) vector-magnetogram data obtained from
Helioseismic and Magnetic Imager. The MI regions for eruptive flares are found
to be strongly localised, whereas the majority of non-eruptive events
($>70~\%$) have scattered imprint regions. To quantify the strength of the MIs,
we derived the integrated change of horizontal field and total change of
Lorentz force over an area. These quantities correlate well with the flare
strength, irrespective of whether flares being eruptive or not, short or long
duration. Further, the free-energy (FE), determined from virial-theorem
estimates, exhibits statistically significant downward trend which starts
around the flare time is observed in majority of flares. The change of FE
during flares do not depend on eruptivity but have a strong positive
correlation ($\approx 0.8$) with the Lorentz force change, indicating that the
part of FE released would penetrate into the photosphere. While these results
strongly favor the idea of significant feedback from corona on the photospheric
magnetic field, the characteristics of MIs are quite indistinguishable for
flares being eruptive or not.
