  The physical mechanisms driving starbursts in dwarf galaxies are unclear, and
the effects of mergers on star formation in these galaxies are still uncertain.
We explore how the merger process affects star formation in metal-poor dwarf
galaxies by analyzing high-spatial-resolution ($\sim$ 70 pc) integral field
spectrograph observations of ionized gas. We use archival data from the Very
Large Telescope/Multi Unit Spectroscopic Explorer to map the spatial
distribution of strong emission lines (e.g., $\rm H\beta$, $\rm H\alpha$, $\rm
[OIII]\lambda5007$, $\rm [NII]\lambda6583$, etc) in the nearby merging
star-forming dwarf galaxy system NGC 4809/4810. We identify approximately 112
star-forming knots scattered among the two galaxies, where the gas-phase
metallicity distribution is inhomogeneous and mixing with metal-poor and
metal-rich ionized gas. Star-forming knots at the interacting region show lower
metallicity, the highest star formation rates (SFRs) and SFR to resolved
main-sequence-relation (rMSR) ratios. Ionized gas exhibits an obvious
northeast-southwest velocity gradient in NGC 4809, while seemingly mixed in NGC
4810. High virial parameters and the stellar mass-size relation of HII regions
indicate that these regions are dominated by direct radiation pressure from
massive stars/clusters and persistently expanding. We find two different
stellar mass surface density-stellar age relations in NGC 4809 and NGC 4810,
and the stellar ages of NGC 4810 are systematically younger than in NGC 4809.
Our study suggests that the merging stage of two dwarf galaxies can induce
starburst activities at the interaction areas, despite the metal-deficient
environment. Considering the high specific SFRs and different stellar ages, we
propose that the interaction initially triggered star formation in NGC 4809 and
then drove star formation in NGC 4810.
