  We have investigated a highly energetic H-ingestion event during shell He
burning leading to H-burning luminosities of $\log(L_\mathrm{H}/\mathrm{\Lsun})
\sim 13$ in a $45 \Msun$ Pop III massive stellar model. In order to track the
nucleosynthesis which may occur in such an event, we run a series of
single-zone nucleosynthesis models for typical conditions found in the stellar
evolution model. Such nucleosynthesis conditions may lead to
$\textit{i}-$process neutron densities of up to $ \sim 10^{13}
\mathrm{cm}^{-3}$. The resulting simulation abundance pattern, where Mg comes
from He burning and Ca from the $\textit{i}$ process, agrees with the general
observed pattern of the most iron-poor star currently known, SMSS
J031300.36-670839.3. However, Na is also efficiently produced in these $i$
process conditions, and the prediction exceeds observations by $\sim 2.5
\unitstyle{dex}$. While this probably rules out this model for SMSS
J031300.36-670839.3, the typical $\textit{i}-$process signature of combined He
burning and $\textit{i}$ process of higher than solar [Na/Mg], [Mg/Al] and low
[Ca/Mg] is reproducing abundance features of the two next most iron-poor stars
HE\,1017-5240 and HE\,1327-2326 very well. The $i$ process does not reach Fe
which would have to come from a low level of additional enrichment.
$\textit{i}$ process in hyper-metal poor or Pop III massive stars may be able
to explain certain abundance patterns observed in some of the most-metal poor
CEMP-no stars.
