  We relate the pre-explosion binding energy of the ejecta of core-collapse
supernovae (CCSNe) of stars with masses in the lower range of CCSNe and the
location of the convection zones in the pre-collapse core of these stars, to
explosion properties in the frame of the jittering jets explosion mechanism.
Our main conclusion is that in the frame of the jittering jets explosion
mechanism the remnant of a pulsar in these low energy CCSNe has some
significance, in that the launching of jets by the newly born neutron star (NS)
spins-up the NS and create a pulsar. We crudely estimated the period of the
pulsars to be tens of milliseconds in these cases. The convective zones seed
perturbations that lead to accretion of stochastic angular momentum that in
turn is assumed to launch jittering jets in this explosion mechanism. We
calculate the binding energy and the location of the convective zones with the
stellar evolution code \textsc{mesa}. For the lowest stellar masses, we study,
$M_{\rm ZAMS} \simeq 8.5-11 M_\odot$, the binding energy above the convective
zones is low, and so is the expected explosion energy in the jittering jets
explosion mechanism that works in a negative feedback cycle. The expected mass
of the NS remnant is $M_{\rm NS} \approx 1.25M_\odot-1.6M_\odot$, even for
these low energy CCSNe.
