Exploring the Energy Sources Powering the Light Curve of the Type Ibn Supernova PS15dpn and the Mass-Loss History of the SN Progenitor

Abstract

PS15dpn is a luminous rapidly rising Type Ibn supernova (SN) discovered by Pan-STARRS1 (PS1). Previous study showed that its bolometric light curve (LC) cannot be explained by the ${}^{56}$Ni model. In this paper, we used the ${}^{56}$Ni model, the magnetar model, the circumstellar interaction (CSI) model, and the CSI plus ${}^{56}$Ni model to fit the bolometric LC of PS15dpn. We found that the ${}^{56}$Ni model can fit the bolometric LC but the parameters are unrealistic, and that the magnetar model, the CSI model, and the CSI plus ${}^{56}$Ni model can match the data with reasonable parameters. Considering the facts that the emission lines indicative of the interaction between the ejecta and the CSM have been confirmed, and that the SNe produced by the explosions of massive stars can synthesize moderate amount of ${}^{56}$Ni, we suggest that the CSI plus ${}^{56}$Ni model is the most promising. Assuming that the CSM is a shell (wind), the masses of the ejecta, the CSM, and the ${}^{56}$Ni are $15.79_{-4.77}^{+5.44}$ M${}_{\odot }$ ($14.18_{-1.64}^{+1.81}$ M${}_{\odot }$), $0.84_{-0.10}^{+0.13}$ M${}_{\odot }$ ($0.88_{-0.12}^{+0.11}$ M${}_{\odot }$), and $0.32_{-0.11}^{+0.11}$ M${}_{\odot }$ ($0.16_{-0.08}^{+0.13}$ M${}_{\odot }$), respectively. The inferred ejecta masses are consistent with the scenario that the progenitors of SNe Ibn are massive Wolf-Rayet stars. Adopting the shell CSM scenario, the shell might be expelled by an eruption of the progenitor just $\sim$ 17$-$167 days prior to the SN explosion; for the wind scenario, the inferred mass-loss rate of the wind is $\sim 8.0$ M${}_{\odot }$ yr${}^{-1}$, indicating that the wind is a "super-wind" having extreme high mass-loss rate.

19 pages, 11 figures, 4 tables, accepted for publication in ApJ

References in corpus (16)

• Physical Properties of Wolf-Rayet Stars
• A giant outburst two years before the core-collapse of a massive star
• Rapidly-Evolving and Luminous Transients from Pan-STARRS1
• SN 2006jc: A Wolf-Rayet Star Exploding in a Dense He-Rich Circumstellar Medium
• Massive stars exploding in a He-rich circumstellar medium. I. Type Ibn (SN 2006jc-like) events
• How much 56Ni can be produced in Core-Collapse Supernovae? : Evolution and Explosions of 30 - 100 Msun Stars
• Analysis of Late--time Light Curves of Type IIb, Ib and Ic Supernovae
• Superluminous Supernovae Powered by Magnetars: Late-time Light Curves and Hard Emission Leakage
• Massive stars exploding in a He-rich circumstellar medium. IV. Transitional Type Ibn Supernovae
• iPTF16asu: A Luminous, Rapidly-Evolving, and High-Velocity Supernova
• Signatures of Circumstellar Interaction in the Unusual Transient AT2018cow
• The Peculiar Type Ib Supernova 2006jc: A WCO Wolf-Rayet Star Explosion
• Type Ibn Supernovae May not all Come from Massive Stars
• A Unified Energy-Reservoir Model Containing Contributions from ${}^{56}$Ni and Neutron Stars and Its Implication to Luminous Type Ic Supernovae
• Massive stars exploding in a He-rich circumstellar medium. V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006
• iPTF14hls as a variable hyper-wind from a very massive star

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• SN 2020bqj: a Type Ibn supernova with a long lasting peak plateau
• Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV bright Underlying Source 2--4 Yr Post-discovery
• Evolution of A Peculiar Type Ibn Supernova SN 2019wep
• Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50--60 Days Post-discovery
• Massive stars exploding in a He-rich circumstellar medium. XI. Diverse evolution of five Ibn SNe 2020nxt, 2020taz, 2021bbv, 2023utc and 2024aej
• Massive stars exploding in a He-rich circumstellar medium $-$ X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt
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