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Some interacting supernovae (SNe) of type IIn show a sizeable continuumpolarisation suggestive of a large scale asymmetry in the circumstellar medium(CSM) and/or the SN ejecta. Here, we extend the recent work of Dessart et al.on super-luminous SNe IIn and perform axially-symmetric (i.e., 2D) multi-groupradiation hydrodynamics simulations to explore the impact of an imposed largescale density asymmetry. When the CSM is asymmetric, the latitudinal variationof the radial optical depth $\tau$ introduces a strong flux redistribution fromthe higher-density CSM regions, where the shock luminosity is larger, towardsthe lower-density CSM regions where photons escape more freely --- thisredistribution ceases when $\tau<$1. Along directions where the CSM density islarger, the shock deceleration is stronger and its progression slower,producing a non-spherical cold-dense shell (CDS). For an oblate CSM densitydistribution, the photosphere (CDS) has an oblate (prolate) morphology when$\tau>$1. When the CSM is symmetric and the ejecta asymmetric, the fluxredistribution within the CSM now tends to damp the latitudinal variation ofthe luminosity at the shock. It then requires a larger ejecta asymmetry toproduce a sizeable latitudinal variation in the emergent flux. When theinteraction is between a SN ejecta and a relic disk, the luminosity boost atearly times scales with the disk opening angle -- forming a super-luminous SNIIn this way requires an unrealistically thick disk. In contrast, interactionwith a disk of modest thickness/mass can yield a power that rivals radioactivedecay of a standard SN II at nebular times.

Two-dimensional radiation-hydrodynamics simulations of super-luminous interacting supernovae of type IIn