2024RAA....24i5009H

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 ⁵⁶Ni model and the ⁵⁶Ni plus circumstellar interaction model fail to explain the LCs, while the four-element (⁵⁶Ni, ⁴⁸Cr, ⁵²Fe, and ⁴⁴Ti) 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 ⁵⁶Ni whose mass is ∼0.03 M_⊙, while the contributions of ⁴⁸Cr and ⁵²Fe can be neglected. The derived ⁴⁴Ti mass (∼0.25 M_⊙) is ∼1.8 times the upper limit of the derived ⁴⁴Ti 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., ⁵⁷Co, ⁵⁵Fe, ⁶⁰Co) can reduce the amount of ⁴⁴Ti, and that this value can be regarded as an upper limit.