  Using MUSE data, we investigate the radial gradients of stellar population
properties (namely age, [M/H], and the abundance ratio of $\alpha$ elements
[$\alpha$/Fe]) for a sample of nine dwarf early-type (dE) galaxies with
log(M$_{\star}$/M$_{\odot}$) $\sim$ 9.0 and an infall time onto the Virgo
cluster of 2-3Gyr ago. We followed a similar approach as in Bidaran et al.
(2022) to derive their stellar population properties and star formation
histories (SFHs) through fitting observed spectral indices and full spectral
fitting, respectively. We find that these nine dE galaxies have truncated
[Mg/Fe]vs.[Fe/H] profiles than equally-massive Virgo dE galaxies with longer
past infall times. Short profiles of three dE galaxies are the result of their
intense star formation which has been quenched long before their accretion onto
the Virgo cluster, possibly as a result of their group environment. In the
remaining six dE galaxies, profiles mainly trace a recent episode of star burst
within 0.4R$_{\rm e}$ which results in higher light-weighted [$\alpha$/Fe]
values. The latter SFH peak can be due to ram pressure exerted by the Virgo
cluster at the time of the accretion of the dE galaxies. Also, we show that
younger, more metal-rich and less $\alpha$-enhanced stellar populations
dominate their inner regions (i.e., < 0.4R$_{\rm e}$) resulting in mainly flat
$\nabla_{\rm age}$, negative $\nabla_{\rm [M/H]}$ and positive $\nabla_{\rm
[\alpha/Fe]}$. We find that with increasing log($\sigma_{\rm Re}$) of dE
galaxies, $\nabla_{\rm age}$ and $\nabla_{\rm [\alpha/Fe]}$ flatten, and the
latter correlation persists even after including early-type galaxies up to
log($\sigma_{\rm Re}$ $\sim$ 2.5), possibly due to the more extended star
formation activity in the inner regions of dEs, as opposed to more massive
early-type galaxies.
