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We present semi-analytical models of galactic outflows in high redshiftgalaxies driven by both hot thermal gas and non-thermal cosmic rays. Thermalpressure alone may not sustain a large scale outflow in low mass galaxies (i.e$M\sim 10^8$~M$_\odot$), in the presence of supernovae (SNe) feedback withlarge mass loading. We show that inclusion of cosmic ray pressure allowsoutflow solutions even in these galaxies. In massive galaxies for the sameenergy efficiency, cosmic ray driven winds can propagate to larger distancescompared to pure thermally driven winds. On an average gas in the cosmic raydriven winds has a lower temperature which could aid detecting it throughabsorption lines in the spectra of background sources. Using our constrainedsemi-analytical models of galaxy formation (that explains the observed UVluminosity functions of galaxies) we study the influence of cosmic ray drivenwinds on the properties of the intergalactic medium (IGM) at differentredshifts. In particular, we study the volume filling factor, averagemetallicity, cosmic ray and magnetic field energy densities for models invokingatomic cooled and molecular cooled halos. We show that the cosmic rays in theIGM could have enough energy that can be transferred to the thermal gas inpresence of magnetic fields to influence the thermal history of theintergalactic medium. The significant volume filling and resulting strength ofIGM magnetic fields can also account for recent $\gamma$-ray observations ofblazars.

Efficient cold outflows driven by cosmic rays in high redshift galaxies and their global effects on the IGM