  We present a Far-Ultraviolet (FUV) study of sixteen star-forming dwarf
galaxies (SFDGs) using the Ultraviolet Imaging Telescope (UVIT).
Morphologically, SFDGs are classified as dwarf spirals, dwarf irregulars, and
blue compact dwarfs (BCDs). We extracted the star-forming complexes (SFCs) from
the sample galaxies, derived their sizes, and estimated the FUV+24$\mu m$ star
formation rates (SFRs). We also determined the approximate stellar disk mass
associated with the SFCs using IRAC 3.6-micron images. We derived the specific
SFRs (sSFRs), as well as the SFR densities ($\Sigma(SFR)$) for the SFCs. We
find that the lower $\Sigma(SFR)$ for each type is different, with the dwarf
irregulars having the lowest $\Sigma(SFR)$ compared to others. However, the
median size of the SFCs in the dwarf irregulars is the largest compared to the
other two types when compared at roughly the same distance. We have derived the
star-forming main sequence (SFMS) on the scale of SFCs for all three classes of
SFDGs. We find that although all SFDGs approximately follow the global SFMS
relation, i.e. $SFR\propto {M_{*}}^{\alpha}$ (where globally $\alpha\approx1$
for low surface brightness galaxies and $0.9$ for SFDGs), on the scale of SFCs
the $\alpha$ value for each type is different. The $\alpha$ values for dwarf
spirals, dwarf irregulars, and BCDs are found to be 0.74$\pm$0.13,
0.8$\pm$0.16, and 0.8$\pm$0.19, respectively. However, the age of all SFCs
approximately corresponds to 1 Gyr. Finally, we find that the outer SFCs in
most galaxies except BCDs have a high sSFR, supporting the inside-out model of
galaxy growth.
