http://arxiv.org/abs/1905.12623
PS15dpn is a luminous rapidly rising Type Ibn supernova (SN) discovered by Pan-STARRS1 (PS1). Previous study shown that the bolometric light curve (LC) cannot be explained by the $^{56}$Ni cascade decay model. In this paper, we employ some alternative models, i.e., the magnetar model, and the $^{56}$Ni plus magnetar model, the ejecta-circumstellar medium (CSM) model (the CSI model), and the CSI plus $^{56}$Ni model, to fit the bolometric LC of PS15dpn. We found that all these models can reproduce the theoretical LCs matching the data. By analyzing the parameters of these models and combining with the spectral features, we conclude that the $^{56}$Ni plus CSI model involving an eruptive shell expelled by the SN progenitor are the most promising one in explaining the LC of PS15dpn. In this scenario, the masses of the ejecta, the CSM, and the $^{56}$Ni are $13.01_{-4.88}^{+4.09}$\,M$\odot$, $0.79{-0.07}^{+0.07}$\,M$\odot$, and $0.35{-0.11}^{+0.08}$\,M$_\odot$, respectively. These parameters are consistent with the conjecture that the progenitors of SNe Ibn are massive Wolf-Rayet stars. Furthermore, our results indicate that the progenitor of PS15dpn might expelled a gas shell $\sim$ 10–230 days prior to the SN explosion.
S. Wang and L. Li
Fri, 31 May 19
45/58
Comments: 8 pages, 2 figures, 2 tables, Submitted to ApJ