  We used the $H\alpha$ images from a large sample of nearby late-type dwarf
galaxies to investigate properties of their emission structure. The sample
consists of three hundred galaxies of the irregular (Irr), Magellanic irregular
(Im), blue compact dwarf (BCD), and transition (Tr) types situated within a
distance of 11 Mpc. In each galaxy, we indicated: the number of compact
HII-regions, the presence of bubble-like or filament-like structures, the
presence of a faint diffuse emission, and a sign of the global burst. The
larger luminosity of a galaxy, the greater number of compact HII-sources in it.
The integral and specific star-formation rates of the dwarf increase steeply
with the increase of the number of HII-regions showing the evidence of the
epidemic character of star-formation process. The dwarf galaxies with
emission-line bubbles, or filaments, or signs of the global star-formation
burst have approximately the same hydrogen-mass-to-luminosity ratio as that of
the whole sample objects. However, their mean star-formation rate is
significantly higher than that of other galaxies in the sample. Emission
bubble-like structures are found in the nearby dwarfs with a frequency of 1
case per 4-5 galaxies. Their linear diameters are close to those expected for
supernova remnants. The mean specific SFR for the nearby late-type dwarfs is
close to the Hubble parameter, $H_0 = -10.14$ dex (yr)$^{-1}$, consistent with
the sluggish cosmic star-formation history of galaxies of this kind.
