Semi-confined supernova feedback in H <scp>ii</scp> region bubbles

ABSTRACT Galactic-scale simulations rely on subgrid models to provide prescriptions for the coupling between supernova (SN) feedback and the interstellar medium (ISM). Many of these models are computed in 1D to allow for an efficient way to account for the variability of properties of their local environment. However, small-scale simulations revealed that the release of energy from SNe within molecular clouds can be highly asymmetrical. This is largely due to the presence of pre-SN feedback, such as ionizing radiation, that are able to carve cavities and channels around the progenitors prior to their detonation. Being partially confined, the SN energy escapes into the outer ISM preferentially through these channels, departing from the spherically symmetric 1D descriptions. To understand by how much the feedback output could differ, we present a theoretical model for a semi-confined SN. The problem concerns a SN expanding into an evolved H ii region, bounded by a molecular cloud with pre-existing vents. With the aid of simple 3D hydrodynamical simulations, we show that this mode of energy release increases the local dynamical impact of the outflows, and extends the time-scales over which the SN is energetically coupled to the surrounding matter. We also show that the amount of small-scale solenoidal turbulence driven by semi-confined SNe may be amplified.