Constraining hydrodynamic model of nearby type IIP SN 2023ixf

Abstract

Despite proximity of SN 2023ixf and a wealth of observational data, the released hydrodynamic models leave too broad range of the derived explosion energy and the ejected mass. We revisit the hydrodynamic modeling based on a broader set of observables than have been previously used. Among those of top priority is the early maximum ejecta velocity that is crucial in removing parameter degeneracy. The inferred parameters of SN 2023ixf are the explosion energy of 2.8x10^{51} erg, ejecta mass of 13.2 Msun, presupernova radius of 1540 Rsun, and Ni-56 mass of 0.07 Msun. The circumstellar matter is composed by the dense circumstellar shell with the mass of 0.01 Msun and radius of 5x10^{14} cm, as well as the external rarefied wind. Both circumstellar components are consistent with the early H-alpha broad wings caused by the Thomson scattering and the intrinsic column density provided by X-ray data. Based on the radiation hydrodynamics we, for the first time, simulate the SN 2023ixf phenomenon from the explosion to the emergence of the hard X-ray radiation.