Type II-Plateau supernova radiation: dependences on progenitor and explosion properties

By L. Dessart, D. John Hillier, R. Waldman, E. Livne. 2013

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We explore the properties of Type II-Plateau (II-P) supernovae (SNe) together with their red supergiant (RSG) star progenitors. Using mesa star, we modulate the parameters (e.g. mixing length, overshoot, rotation, metallicity) that control the evolution of a 15 M-circle dot main-sequence star to produce a variety of physical pre-SN models and SN II-P ejecta. We extend previous modelling of SN II-P radiation to include photospheric and nebular phases, as well as multiband light curves and spectra. Our treatment does not assume local thermodynamic equilibrium, is time dependent, treats explicitly the effects of line blanketing and incorporates non-thermal processes. We find that the colour properties of SNe II-P require large model atoms for Fe i and Fe ii, much larger than previously adopted. The colour properties also imply RSG progenitors of limited extent (similar to 500 R-circle dot) - larger progenitor stars produce an SN II-P radiation that remains too blue for too long. This finding calls for a reduction of RSG radii, perhaps through a strengthening of convective energy transport in RSG envelopes. Increased overshoot and rotation reduce the ratio of ejecta to helium-core mass, similarly to an increase in main-sequence mass, and thus complicate the inference of progenitor masses. In contrast to the great sensitivity on progenitor radius, SN II-P colour evolution appears insensitive to variations in explosion energy. Finally, we document the numerous SN II-P signatures that vary with progenitor metallicity, revealing their potential for metallicity determinations in the nearby and distant Universe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/48f9e166b2cf5ed666e8efa03927f7d6784b4f92

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Citations in the corpus

• The diversity of Type II supernova versus the similarity in their progenitors (2016, methodology): “…et al. 2014 for a discussion), and spectral synthesis modeling has been widely used to constrain the abundance of different elements in the ejecta (Mazzali et al. 2007, 2010; Dessart & Hillier 2010; Dessart et al. 2013; Jerkstrand et al. 2012, 2015a,b) and to elucidate the nature of the progenitor.”
• CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, background): “We also note that Dessart et al. (2013) analyzed the dependencies of SN IIP radiation on progenitor and explosion properties.”
• Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “As a consequence, fitting the early SNII light curves with the analytical and numerical models resulted in relatively small (∼500 R) estimated radii of their progenitors (Dessart et al. 2013; González-Gaitán et al. 2015; Garnavich et al. 2016; see, however, Rubin et al. 2016; Shussman et al. 2016).”
• Low luminosity Type II supernovae - II. Pointing towards moderate mass precursors (2014, background): “Dessart et al. (2013) suggested it may be related to the pre-SN structure being not well understood.”
• THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “Often, the modeled ejecta masses (and thus possibly also the explosion energies) are overestimated (e.g. Utrobin 2007; Utrobin & Chugai 2009; Dessart & Hillier 2011; Dessart et al. 2013).”
• Pre-supernova outbursts via wave heating in massive stars – I. Red supergiants (2017, background): “When the shock wave breaks out of the surface, it produces a sudden spike in surface temperature and luminosity (see Figs 8 and 9), akin to SN shock breakout (Dessart et al. 2013) but MNRAS 470, 1642–1656 (2017) with much smaller energy, E ∼ 1047 erg.”
• The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines (2013, background): “Models with overshooting produce about twice as much oxygen as models without and fast-rotating models produce a factor ∼1.5 more oxygen than non-rotating ones (Dessart et al. 2013).”
• TOWARD CHARACTERIZATION OF THE TYPE IIP SUPERNOVA PROGENITOR POPULATION: A STATISTICAL SAMPLE OF LIGHT CURVES FROM Pan-STARRS1 (2014, methodology): “However, the Dessart et al. (2013) grid was limited to a single initial progenitor mass of 15 M .”