The explosion of 9$-$29$M_\odot$ stars as Type II supernovae : results from radiative-transfer modeling at one year after explosion

TL;DR

This study models one-year-old Type II supernovae using radiative transfer calculations based on detailed explosion models, revealing how spectral lines relate to progenitor mass and explosion properties, and comparing results with observed supernovae.

Contribution

It provides the first comprehensive radiative transfer modeling of one-year-old Type II supernovae across a range of progenitor masses, connecting spectral features to progenitor characteristics.

Findings

[OI] line flux increases with progenitor mass

Hα line exhibits an opposite trend to [OI]

Spectral features can estimate progenitor mass within 12-15 M_sun

Abstract

We present a set of nonlocal thermodynamic equilibrium steady-state calculations of radiative transfer for one-year old type II supernovae (SNe) starting from state-of-the-art explosion models computed with detailed nucleosynthesis. This grid covers single-star progenitors with initial masses between 9 and 29$M_{\odot}$, all evolved with KEPLER at solar metallicity and ignoring rotation. The [OI]$\lambda\lambda$$6300,6364$ line flux generally grows with progenitor mass, and H$\alpha$ exhibits an equally strong and opposite trend. The [CaII]$\lambda\lambda$$7291,\,7323$ strength increases at low $^{56}$Ni mass, low explosion energy, or with clumping. This CaII doublet, which forms primarily in the explosively-produced Si/S zones, depends little on the progenitor mass, but may strengthen if Ca$^+$ dominates in the H-rich emitting zones or if Ca is abundant in the O-rich zones. Indeed, Si-O shell merging prior to core collapse may boost the CaII doublet at the expense of the OI doublet, and may thus mimic the metal line strengths of a lower mass progenitor. We find that the $^{56}$Ni bubble effect has a weak impact, probably because it is too weak to induce much of an ionization shift in the various emitting zones. Our simulations compare favorably to observed SNe II, including SN2008bk (e.g., 9$M_{\odot}$ model), SN2012aw (12$M_{\odot}$ model), SN1987A (15$M_{\odot}$ model), or SN2015bs (25$M_{\odot}$ model with no Si-O shell merging). SNe II with narrow lines and a low $^{56}$Ni mass are well matched by the weak explosion of 9$-$11$M_{\odot}$ progenitors. The nebular-phase spectra of standard SNe II can be explained with progenitors in the mass range 12$-$15$M_{\odot}$, with one notable exception for SN2015bs. In the intermediate mass range, these mass estimates may increase by a few $M_{\odot}$ with allowance for clumping of the O-rich material or CO molecular cooling.