  The recent history of star formation in the BCD galaxy VII Zw403, is analysed
with accounts for the dynamics of the remnant generated either by an
instantaneous burst or by a continuous star formation event.
  We have re-observed VII Zw403 with a better sensitivity corresponding to the
threshold H$_{\alpha}$ flux $8.15 \times 10^{-17}$ erg cm$^{-2}$ s$^{-1}$. The
total H$_{\alpha}$ luminosity derived from our data is much larger than
reported before, and presents a variety of ionized filaments and incomplete
shells superimposed on the diffuse H$_{\alpha}$ emission. This result has a
profound impact on the predicted properties of the starburst blown superbubble.
Numerical calculations based on the previous H$_{\alpha}$ data, predict two
different scenarios of star formation able to match simultaneously all observed
parameters. These are an instantaneous burst of star formation with a total
mass of $5 \times 10^5$ M$_{\odot}$ and a star-forming event with a constant
SFR = $4 \times 10^{-3}$ M$_{\odot}$ yr$^{-1}$, which lasts for 35 Myrs. The
numerical calculations based on the energy input rate derived from our
observations predict a short episode of star formation lasting less than 10
Myrs with a total star cluster mass $\sim (1 - 3) \times 10^6$ M$_{\odot}$.
