PS15dpn is a luminous rapidly rising Type Ibn supernova ( SN ) discovered by Pan-STARRS1 ( PS1 ) .
Previous study shown that the bolometric light curve ( LC ) can not 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 .