Exploring the Energy Sources Powering the Light Curve of the Type Ibn Supernova PS15dpn and the Mass-Loss History of the SN Progenitor. (arXiv:1905.12623v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Shan-Qin Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">Long Li</a>
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.
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.
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