  We investigate surface brightness profiles (SBPs) of dwarf galaxies in field,
group, and cluster environments. With deep $BVI$ images from the Korea
Microlensing Telescope Network Supernova Program, SBPs of 38 dwarfs in the NGC
2784 group are fitted by a single exponential or double exponential model. We
find that 53% of the dwarfs are fitted with single exponential profiles ("Type
I"), while 47% of the dwarfs show double exponential profiles. 37% of all
dwarfs have smaller sizes of the outer part than inner part ("Type II"), while
10% have a larger sized outer than inner part ("Type III"). We compare these
results with those in the field and in the Virgo cluster, where SBP types of
102 field dwarfs are compiled from a previous study and SBP types of 375
cluster dwarfs are measured using SDSS $r$-band images. As a result, the
distributions of SBP types are different in three environments. Common SBP
types of the field, the NGC 2784 group, and the Virgo cluster are Type II, Type
I and II, and Type I and III profiles, respectively. After comparing sizes of
dwarfs in different environments, we suggest that since sizes of some dwarfs
are changed due to the environmental effects, SBP types are able to be
transformed and the distributions of SBP types in three environments are
different. We discuss possible environmental mechanisms on the transformation
of SBP types.
