  Certain types of silicon carbide (SiC) grains, e.g., SiC-X grains, and low
density (LD) graphites are C-rich presolar grains that are thought to have
condensed in the ejecta of core-collapse supernovae (CCSNe). In this work we
compare C, N, Al, Si, and Ti isotopic abundances measured in presolar grains
with the predictions of 21 CCSN models. The impact of a range of SN explosion
energies is considered, with the high energy models favouring the formation of
a C/Si zone enriched in $^{12}$C, $^{28}$Si, and $^{44}$Ti. Eighteen of the 21
models have H ingested into the He-shell and different abundances of H
remaining from such H-ingestion. CCSN models with intermediate to low energy
(that do not develop a C/Si zone) cannot reproduce the $^{28}$Si and $^{44}$Ti
isotopic abundances in grains without assuming mixing with O-rich CCSN ejecta.
The most $^{28}$Si-rich grains are reproduced by energetic models when material
from the C/Si zone is mixed with surrounding C-rich material, and the observed
trends of the $^{44}$Ti/$^{48}$Ti and $^{49}$Ti/$^{48}$Ti ratios are consistent
with the C-rich C/Si zone. For the models with H-ingestion, high and
intermediate explosion energies allow the production of enough $^{26}$Al to
reproduce the $^{26}$Al/$^{27}$Al measurements of most SiC-X and LD graphites.
In both cases, the highest $^{26}$Al/$^{27}$Al ratio is obtained with H still
present at $X_H \approx 0.0024$ in He-shell material when the SN shock is
passing. The existence of H in the former convective He-shell points to late
H-ingestion events in the last days before massive stars explode as a
supernova.
