  In the standard paradigm, satellite galaxies are believed to be associated
with the population of dark matter subhalos. In this paper, we use the
conditional stellar mass functions of {\it satellite galaxies} obtained from a
large galaxy group catalogue together with models of the subhalo mass functions
to explore the fraction and fate of stripped stars from satellites in galaxy
groups and clusters of different masses. The majority of the stripped stars in
massive halos are predicted to end up as intra-cluster stars, and the predicted
amounts of the intra-cluster component as a function of the velocity dispersion
of galaxy system match well the observational results obtained by Gonzalez et
al. (2007). The fraction of the mass in the stripped stars to that remain bound
in the central and satellite galaxies is the highest ($\sim 40%$ of the total
stellar mass) in halos with masses $M_h\sim 10^{14}\msunh$. If all these stars
end up in the intra-cluster component (Max), or maximum of them are accreted
into the central galaxy (Min), then we can predict that a maximum $\sim 19%$
and a minimum $\sim 5%$ of the total stars in the whole universe are in terms
of the diffused intra-cluster component. In the former case, in massive halos
with $M_h \sim 10^{15} \msunh$, the stellar mass of the intra-cluster component
is roughly 6 times as large as that of the central galaxy. This factor
decreases to $\sim 2$, 1 and 0.1 in halos with $M_h \sim 10^{14}$, $10^{13}$,
and $10^{12} \msunh$, respectively. The total amount of stars stripped from
satellite galaxies is insufficient to build up the central galaxies in halos
with masses $\la 10^{12.5}\msunh$, and so the quenching of star formation must
occur in halos with higher masses. Abridged.
