Star formation properties in the Local Volume galaxies via $H\alpha$ and
  FUV fluxes
  A distance-limited sample of 869 objects from the Updated Nearby Galaxy
Catalog is used to characterize the star formation status of the Local Volume
population. We present a compiled list of 1217 star formation rate (SFR)
estimates for 802 galaxies within 11 Mpc from us, derived from the H-alpha
imaging surveys and GALEX far-ultraviolet survey. We briefly discuss some basic
scaling relations between SFR and luminosity, morphology, HI-mass, surface
brightness, as well as environment of the galaxies. About 3/4 of our sample
consist of dwarf galaxies, for which we offer a more refined classification. We
note that the specific star formation rate of nearly all luminous and dwarf
galaxies does not exceed the maximum value: $\log(SFR/L_K) = -9.4$ [yr$^{-1}$].
The bulk of spiral and blue dwarf galaxies have enough time to generate their
stellar mass during the cosmological time, $T_0$, with the observed SFRs. They
dispose of a sufficient amount of gas to support their present SFRs over the
next $T_0$ term. We note that only a minor part of BCD, Im, and Ir galaxies
(about 1/20) proceeds in a mode of vigorous star-burst activity. In general,
the star formation history of spiral and blue dwarf galaxies is mainly driven
by their internal processes. The present SFRs of E, S0 and dSph galaxies are
typically (1/30 - 1/300) of their former activity.
