The Energy Sources and the Explosion Mechanism of Ca-rich supernova PTF~10iuv

In this paper, we perform the detailed modeling for the light curves (LCs) of PTF 10iuv which is a calcium-rich (Ca-rich) supernova (SN) to constrain the physical properties of its ejecta and the energy sources, as well as the explosion mechanism. We find that the 56 Ni model and the 56 Ni plus circumstellar interaction model fail to explain the LCs, while the four-element ( 56 Ni, 48 Cr, 52 Fe, and 44 Ti) model can account for the LCs. The ejecta mass of PTF 10iuv derived by the model ( 1.52 − 0.25 + 0.34 M ⊙ ) is consistent with that of the merger of a sub-Chandrasekhar mass white dwarf. The early-time LCs were mainly powered by 56 Ni whose mass is ∼0.03 M ⊙ , while the contributions of 48 Cr and 52 Fe can be neglected. The derived 44 Ti mass (∼0.25 M ⊙ ) is ∼1.8 times the upper limit of the derived 44 Ti mass of Ca-rich SN 2005E. We suggest that subtracting the contributions of the host-galaxy, which are unknown, and including the flux from other long-lived elements (e.g., 57 Co, 55 Fe, 60 Co) can reduce the amount of 44 Ti, and that this value can be regarded as an upper limit.