We model how repeated supernova explosions in high-redshift dwarf starburst galaxies drive superbubbles and winds out of the galaxies .
We compute the efficiencies of metal and mass ejection and energy transport from the galactic potentials , including the effect of cosmological infall of external gas .
The starburst bubbles quickly blow out of small , high-redshift , galactic disks , but must compete with the ram pressure of the infalling gas to escape into intergalactic space .
We show that the assumed efficiency of the star formation rate dominates the bubble evolution and the metal , mass , and energy feedback efficiencies .
With star formation efficiency f _ { * } = 0.01 , the ram pressure of infall can confine the bubbles around high-redshift dwarf galaxies with circular velocities v _ { c } \gtrsim 52 km s ^ { -1 } .
We can expect high metal and mass ejection efficiencies , and moderate energy transport efficiencies in halos with v _ { c } \approx 30 - 50 km s ^ { -1 } 
and f _ { * } \approx 0.01 as well as in halos with v _ { c } \approx 100 km s ^ { -1 } 
and f _ { * } \gg 0.01 .
Such haloes collapse successively from 1–2 \sigma peaks in \Lambda CDM Gaussian density perturbations as time progresses .
These dwarf galaxies can probably enrich low and high-density regions of intergalactic space with metals to 10 ^ { -3 } – 10 ^ { -2 } Z _ { \odot } 
as they collapse at z \approx 8 and z \lesssim 5 respectively .
They also may be able to provide adequate turbulent energy to prevent the collapse of other nearby halos , as well as to significantly broaden Lyman- \alpha absorption lines to v _ { rms } \approx 20 –40 km s ^ { -1 } .
We compute the timescales for the next starbursts if gas freely falls back after a starburst , and find that , for star formation efficiencies as low as f _ { * } \lesssim 0.01 , the next starburst should occur in less than half the Hubble time at the collapse redshift .
This suggests that episodic star formation may be ubiquitous in dwarf galaxies .