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Molecular outflows contributing to the matter cycle of star forming galaxiesare now observed in small and large systems at low and high redshift. Theirphysical origin is still unclear. In most theoretical studies only warmionised/neutral and hot gas outflowing from the interstellar medium isgenerated by star formation. We investigate an in-situ H$_2$ formation scenarioin the outflow using high-resolution simulations, including non-equilibriumchemistry and self-gravity, of turbulent, warm, and atomic clouds withdensities 0.1, 0.5 and $1\,\mathrm{cm}^{-3}$ exposed to a magnetised hot wind.For cloud densities $\gtrsim 0.5\,\mathrm{cm}^{-3}$ a magnetised wind triggersH$_2$ formation before cloud dispersal. Up to 3 per cent of the initial cloudmass can become molecular on $\sim 10\,\mathrm{Myr}$ time scales. The effect isstronger for winds with perpendicular $B$-fields and intermediate densityclouds ($n_\mathrm{c}\sim 0.5\,\mathrm{cm}^{-3}$). Here H$_2$ formation can beboosted by up to one order of magnitude compared to isolated cooling cloudsindependent of self-gravity. Self-gravity preserves the densest clouds way pasttheir $\sim 15\,\mathrm{Myr}$ cloud crushing time scales. This model couldprovides a plausible in-situ origin for the observed molecular gas. Warmionised gas is also generated, almost independent of the cloud density. Theamount solely depend on the magnetic field configuration in the wind. For lowdensity clouds ($0.1\,\mathrm{cm}^{-3}$), the forming warm ionised gas can beas much as 60 per cent of the initially atomic cloud mass. This couldcontribute to observations of outflows with ionised gas sensitive tracers.

The in situ formation of molecular and warm ionised gas triggered by hot outflows