Radiative-transfer modeling of nebular-phase type II supernovae. Dependencies on progenitor and explosion properties

TL;DR

This study models nebular-phase spectra of type II supernovae to understand how progenitor and explosion properties influence observable features, highlighting the importance of 56Ni mixing and progenitor mass signatures.

Contribution

It introduces a set of 1-D radiative transfer models for type II SNe at 300 days post-explosion, exploring dependencies on progenitor mass, 56Ni mixing, and chemical composition.

Findings

OI6300 doublet strength correlates with progenitor mass

Spectra are sensitive to 56Ni mixing and distribution

Convective shell merging can weaken OI emission in nebular spectra

Abstract

Nebular phase spectra of core-collapse supernovae (SNe) provide critical and unique information on the progenitor massive star and its explosion. We present a set of 1-D steady-state non-local thermodynamic equilibrium radiative transfer calculations of type II SNe at 300d after explosion. Guided by results for a large set of stellar evolution simulations, we craft ejecta models for type II SNe from the explosion of a 12, 15, 20, and 25Msun star. The ejecta density structure and kinetic energy, the 56Ni mass, and the level of chemical mixing are parametrized. Our model spectra are sensitive to the adopted line Doppler width, a phenomenon we associate with the overlap of FeII and OI lines with Lyalpha and Lybeta. Our spectra show a strong sensitivity to 56Ni mixing since it determines where decay power is absorbed. Even at 300d after explosion, the H-rich layers reprocess the radiation from the inner metal rich layers. In a given progenitor model, variations in 56Ni mass and distribution impact the ejecta ionization, which can modulate the strength of all lines. Such ionization shifts can quench CaII line emission. In our set of models, the OI6300 doublet strength is the most robust signature of progenitor mass. However, we emphasize that convective shell merging in the progenitor massive star interior can pollute the O-rich shell with Ca, which will weaken the OI6300 doublet flux in the resulting nebular SN II spectrum. This process may occur in Nature, with a greater occurrence in higher mass progenitors, and may explain in part the preponderance of progenitor masses below 17Msun inferred from nebular spectra.