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Molecular cloud structure is regulated by stellar feedback in various forms.Two of the most important feedback processes are UV photoionisation andsupernovae from massive stars. However, the precise response of the cloud tothese processes, and the interaction between them, remains an open question. Inparticular, we wish to know under which conditions the cloud can be dispersedby feedback, which in turn can give us hints as to how feedback regulates thestar formation inside the cloud. We perform a suite of radiativemagnetohydrodynamic simulations of a 10^5 solar mass cloud with embeddedsources of ionising radiation and supernovae, including multiple supernovae anda hypernova model. A UV source corresponding to 10% of the mass of the cloud isrequired to disperse the cloud, suggesting that the star formation efficiencyshould be on the order of 10%. A single supernova is unable to significantlyaffect the evolution of the cloud. However, energetic hypernovae and multiplesupernovae are able to add significant quantities of momentum to the cloud,approximately 10^{43} g cm/s of momentum per 10^{51} ergs of supernova energy.This is on the lower range of estimates in other works, since dense gas clumpsthat remain embedded inside the HII region cause rapid cooling in the supernovablast. We argue that supernovae alone are unable to regulate star formation inmolecular clouds, and that strong pre-supernova feedback is required to allowsupernova blastwaves to propagate efficiently into the interstellar medium

Feedback in Clouds II: UV Photoionisation and the first supernova in a massive cloud