Abstract The direct method for determining cosmological distances uses observations at the growth stage of the luminosity of superluminous supernovae, whose light curve can be explained by the interaction of a shock wave with dense circumstellar matter. The method is based on the assumption of spherical symmetry of the dense thin layer formed in the system, which can be unstable in a multidimensional model. In this paper, we consider the simulation of the supernova SN2009ip, which has been successfully applied for the direct method, using the radiation-hydrodynamics code, FRONT. It is shown that the current implementation of the code correctly reproduces the bolometric light curve and the dynamics of the dense shell’s motion in a simplified SN2009ip model. It is also shown that in the formulation under consideration, the shell remains spherically symmetric at least during the growth period of the light curve.
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