  In an earlier paper, we determined the morphological types of galaxies in the
Coma Cluster using data from the HST/ACS Coma Cluster treasury survey. We found
that of the 132 members, 51 are non dwarfs and 81 are dwarfs. We define dwarfs
to have a absolute luminosity $M_{F814W}\geq -18.5$ as in
\cite{2012ApJ...746..136M}.
  In this paper, we determine the morphological types of these dwarf galaxies
and make a detailed study of their properties. Using GALFIT, we determine the
structural properties of our sample and with spectroscopic redshifts, we
determined memberships and distances to identify dwarfs. A visual examination
of the residual images reveals that our sample of 78 dwarf galaxies comprises
of: dwarf lenticular (\textit{dS0}) 22\%, dwarf Elliptical ($dE$) 69\%, dwarf
spirals (\textit{dSp}) 4\%, dwarf ring (\textit{dring}) 1\%, dwarf barred
spirals (\textit{dSBp}) 3\% and dwarf irregular (\textit{dIrr}) 1\% galaxies.
We find that the bulge-disk decomposition (S\'ersic + exponential) fits are
good only for the \textit{dS0} galaxies. The remainder of the sample gives good
fits only for single S\'ersic fits. The Colour Magnitude Relation (CMR) shows
that the $dEs$ are redder and fainter than the rest of the sample (except one
$dIrr$ galaxy). The Kormendy relation reveals that $dE$ galaxies have lower
surface brightness than the rest of the sample. Our research leads us to the
conclusion that dwarf galaxies appear to have a different formation and
evolution process than non-dwarf galaxies.
