  We calculate the nucleosynthesis inside the hot bubble formed in the
jittering-jets model for core collapse supernovae (CCSNe) explosions, and find
the formation of several times 10^-4 M_\odot of r-process elements. In the
jittering-jets model fast jets launched from a stochastic accretion disk around
the newly formed neutron star are shocked at several thousands km, and form hot
high-pressure bubbles. These bubbles merge to form a large bubble that explode
the star. In the current study we assume a spherically symmetric homogenous
bubble, and follow its evolution for about one second during which nuclear
reactions take place. The jets last for about one second, their velocity is
v_j=0.5c, and their total energy is 10^51 erg. We use jets' neutron enrichment
independent on time, and follow the nuclear reactions to the formation of the
seed nuclei up to $Z \leq 50$, on which more neutrons will be absorbed to form
the r-process elements. Based on the mass of the seed nuclei we find the
r-process element mass in our idealized model to be several times 10^-4
M_\odot, which is slightly larger than the value deduced from observations.
More realistic calculations that relax the assumptions of a homogenous bubble
and constant jets composition might lead to agreement with observations.
