We present simulations of the magnetized interstellar medium ( ISM ) in models of massive star forming ( 40 \hbox { $ \mathrm { \thinspace M _ { \odot } } $ } { \thinspace yr } ^ { -1 } ) disk galaxies with high gas surface densities ( \Sigma _ { \mathrm { gas } } \sim 100 \hbox { $ \mathrm { \thinspace M _ { \odot } } $ } { % \thinspace pc } ^ { -2 } ) similar to observed star forming high-redshift disks .
We assume that type II supernovae deposit 10 per cent of their energy into the ISM as cosmic rays and neglect the additional deposition of thermal energy or momentum .
With a typical Galactic diffusion coefficient for CRs ( 3 \mbox { \textperiodcentered } 10 ^ { 28 } \mathrm { c } \mathrm { m } ^ { 2 } { \thinspace s% } ^ { -1 } ) we demonstrate that this process alone can trigger the local formation of a strong low density galactic wind maintaining vertically open field lines .
Driven by the additional pressure gradient of the relativistic fluid the wind speed can exceed 10 ^ { 3 } { \thinspace km \thinspace s } ^ { -1 } , much higher than the escape velocity of the galaxy .
The global mass loading , i.e .
the ratio of the gas mass leaving the galactic disk in a wind to the star formation rate becomes of order unity once the system has settled into an equilibrium .
We conclude that relativistic particles accelerated in supernova remnants alone provide a natural and efficient mechanism to trigger winds similar to observed mass-loaded galactic winds in high-redshift galaxies .
These winds also help explaining the low efficiencies for the conversion of gas into stars in galaxies as well as the early enrichment of the intergalactic medium with metals .
This mechanism can be at least of similar importance than the traditionally considered momentum feedback from massive stars and thermal and kinetic feedback from supernova explosions .