A Unified Energy-Reservoir Model Containing Contributions from ${}^{56}$Ni and Neutron Stars and Its Implication to Luminous Type Ic Supernovae

Abstract

Most type-Ic core-collapse supernovae (CCSNe) produce ${}^{56}$Ni and neutron stars (NSs) or black holes (BHs). The dipole radiation of nascent NSs has usually been neglected in explaining supernovae (SNe) with peak absolute magnitude $M_{\mathrm{peak}}$ in any band are $\gtrsim -19.5$~mag, while the ${}^{56}$Ni can be neglected in fitting most type-Ic superluminous supernovae (SLSNe Ic) whose $M_{\mathrm{peak}}$ in any band are $\lesssim -21$~mag, since the luminosity from a magnetar (highly magnetized NS) can outshine that from a moderate amount of ${}^{56}$Ni. For luminous SNe Ic with $-21\lesssim M_{\mathrm{peak}}\lesssim -19.5$~mag, however, both contributions from ${}^{56}$Ni and NSs cannot be neglected without serious modeling, since they are not SLSNe and the ${}^{56}$Ni mass could be up to $\sim 0.5M_{\odot }$. In this paper we propose a unified model that contain contributions from both ${}^{56}$Ni and a nascent NS. We select three luminous SNe Ic-BL, SN~2010ay, SN~2006nx, and SN~14475, and show that, if these SNe are powered by ${}^{56}$Ni, the ratio of $M_{\mathrm{Ni}}$ to $M_{\mathrm{ej}}$ are unrealistic. Alternatively, we invoke the magnetar model and the hybrid (${}^{56}$Ni + NS) model and find that they can fit the observations, indicating that our models are valid and necessary for luminous SNe Ic. Owing to the lack of late-time photometric data, we cannot break the parameter degeneracy and thus distinguish among the model parameters, but we can expect that future multi-epoch observations of luminous SNe can provide stringent constraints on ${}^{56}$Ni yields and the parameters of putative magnetars.

arXiv comment24 pages, 1 table, 2 figures, accepted for publication in ApJ

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