tokens: with the wind. Fig. 15 shows the time evolution of the WIM for all simulations with self-gravity. We note that the main parameter that changes the total amount of the WIM is not the density of the cloud but mainly the magnetic field properties in the wind. All winds with a perpendicular field keep the clouds mostly intact due to the magnetic draping effect and reduce the mixing of warm atomic and hot ionized gas at the cloud–wind interface. The resulting mass in the WIM converges after about 10 Myr of evolution to give . For the non-magnetic wind, the masses converge after at a value of . The highest masses in the WIM are reached for with about . We highlight that this is 60 per cent of the initial mass of the low-density cloud. The parallel field configuration delays or completely suppresses the contraction perpendicular to the magnetic field and thereby maximizes the mixing that leads to the WIM. Figure 15. Time evolution of the warm ionized gas. The total mass mainly depends on the the wind properties rather than the cloud mass. We show only the low density up to the point of their destruction and their transport through the right-hand boundary. We find the lowest mass in , followed by the non-magnetic wind. For , the warm ionized mass is largest. 8 DISCUSSION AND CONCLUSIONS 8.1 Cloud survival For clouds exposed to a wind, the question arises whether the clouds are fed by condensation of wind material and grow, whether they are effectively unaltered, or whether the wind eventually disrupts the cloud. In absence of stabilizing mechanisms, the clouds are likely to be destroyed by the efficient growth of the Rayleigh–Taylor instability and the shear-driven Kelvin–Helmhotz instability (Cooper et al. 2009 ; Scannapieco Brüggen 2015 ; Schneider Robertson 2015 , 2017 ). Stabilizing mechanisms can be the cooling and a resulting contraction that reduces the effective interaction cross-section with the wind. It could also be the magnetic field configuration, which suppresses instabilities or – mostly for dense clouds – self-gravity, which leads to faster contraction and even collapse. Cooling can lead to fragmentation of the clouds (McCourt et al. 2018 ) but can also help to stabilize them by suppressing the mixing (Sparre et al. 2019 ). Stabilized condensations can grow in mass due to newly accreted gas from the wind (Marinacci et al. 2010 ; Armillotta, Fraternali Marinacci 2016 ; Armillotta et al. 2017 ; Gronke Oh 2018 , 2020 ). Magnetic fields help to keep the gas confined and increase the acceleration efficiency (McCourt et al. 2015 ; Banda-Barragán et al. 2016 , 2018 , 2019 ; Grønnow et al. 2018 ; Sparre, Pfrommer Ehlert 2020 ). All of the above-mentioned simulations have focused on overall lower densities and higher temperatures compared to this study. However, the surviving fragments develop strong density fluctuations, which are comparable to the initial configurations in our models. We evolve the systems for a time-scale of a few
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