  We examine the connections between the current global star formation
activity, luminosity, dynamical mass and morphology of galaxies in the Local
Volume, using H-alpha data from the 11 Mpc H-alpha and Ultraviolet Galaxy
Survey (11HUGS). Taking the equivalent width (EW) of the H-alpha emission line
as a tracer of the specific star formation rate, we analyze the distribution of
galaxies in the M_B-EW and rotational velocity (V_{max})-EW planes.
Star-forming galaxies show two characteristic transitions in these planes. A
narrowing of the galaxy locus occurs at M_B~-15 and V_{max}~50 km/s, where the
scatter in the logarithmic EWs drops by a factor of two as the
luminosities/masses increase, and galaxy morphologies shift from predominately
irregular to late-type spiral. Another transition occurs at M_B~-19 and
V_{max}~120 km/s, above which the sequence turns off toward lower EWs and
becomes mostly populated by intermediate and early-type bulge-prominent
spirals. Between these two transitions, the mean logarithmic EW appears to
remain constant at 30 A. We comment on how these features reflect established
empirical relationships, and provide clues for identifying the large-scale
physical processes that both drive and regulate star formation, with emphasis
on the low-mass galaxies that dominate our approximately volume-limited sample.
