Supernovae from red supergiants with extensive mass loss

By T. Moriya, Nozomu Tominaga, S. Blinnikov, P. Baklanov, E. Sorokina. 2010

133 citations recorded by the source corpus.

We calculate multicolour light curves (LCs) of supernovae (SNe) from red supergiants (RSGs) that have exploded within a dense circumstellar medium (CSM). Multicolour LCs are calculated by using the multigroup radiation hydrodynamics code STELLA. If the CSM is dense enough, the shock breakout signal is delayed and smeared by the CSM and the kinetic energy of SN ejecta is efficiently converted to thermal energy, which is eventually released as radiation. We find that explosions of RSGs are affected by the CSM in the early epochs, when the mass-loss rate just before the explosions is higher than ∼10 ―4 M ⊙ yr ―1 . Their characteristic features are that the LC has a luminous round peak followed by a flat part, that multicolour LCs are simultaneously bright in both ultraviolet and optical at the peak, and that the photo-spheric velocity is very low at these epochs. We calculate LCs for various CSM conditions and explosion properties, i.e. mass-loss rates, radii of the CSM, density slopes of the CSM, explosion energies of SN ejecta and the SN progenitors contained within, to see their influence. We compare our model LCs with those of ultraviolet-bright Type IIP SN 2009kf and show that the mass-loss rate of the progenitor of SN 2009kf just before the explosion is likely to be higher than 10- 4 M ⊙ yr ―1 . Combined with the fact that SN 2009kf is likely to be an energetic explosion and has large 56 Ni production, which implies that the progenitor of SN 2009kf is a massive RSG, our results indicate that there could be some mechanism to induce extensive mass loss in massive RSGs just before their explosions.

View Paper: https://www.semanticscholar.org/paper/b292de6e4643befedac12206a0011a10c5aaa8d1

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Citations in the corpus

• Pre-supernova outbursts via wave heating in massive stars – I. Red supergiants (2017, background): “In this paper, we examine wave heating effects in otherwise ‘typical’ MZAMS = 15 M red supergiants (RSGs) that may give rise to Type II-P, II-L or IIn SNe depending on the impact of wave heating.”
• Unifying Type II Supernova Light Curves with Dense Circumstellar Material (2016, methodology): “In contrast, for example, Moriya et al. (2011) considers larger radii (∼ 104R ) and wind mass loss rates in the range of 10−4 − 10−2M yr−1.”
• Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, methodology): “We also note that a systematic study of the effect of CSM properties on LCs powered by the interaction between SN ejecta and dense CSM is summarized in Moriya et al. (2011).”
• SHOCK BREAKOUT IN DENSE MASS LOSS: LUMINOUS SUPERNOVAE (2011, methodology): “Substituting the parameters into equation (5), the radiated energy is Erad = 1.4 × 1050 ergs, which is close to the 2.0 × 1050 ergs found in the numerical model (Moriya et al. 2010).”
• ANALYTICAL LIGHT CURVE MODELS OF SUPERLUMINOUS SUPERNOVAE: χ2-MINIMIZATION OF PARAMETER FITS (2013, methodology): “Radiation hydrodynamics simulations of interactions of SN ejecta with massive CSM shells of various power-law density profiles (Moriya et al. 2011; 2012, Ginzburg & Balberg 2012) provided important insights to the dependence of the main features of the resulting numerical LCs on the model…”
• Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “In this case, the shock breaks out inside the wind, which changes the timescale of the breakout from the expected hours to days (Moriya et al. 2011).”
• HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, methodology): “The temperature is taken to decrease from 2 × 104 K to 1 × 104 K, similar to what is found in detailed simulations of shocks (e.g., Figure 6 in Moriya et al. 2011), as well as from our photoionization calculations in Sect.”
• GENERALIZED SEMI-ANALYTICAL MODELS OF SUPERNOVA LIGHT CURVES (2011, methodology): “Bolometric and color LCs of SNe produced by the interaction of SN ejecta (from a RSG progenitor) with a CSM that is a steady state wind (s = 2) or with a s = 1.5 density profile slope were presented by Moriya et al. (2011) as results of 1-”
• Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “Moriya et al. (2011) reached similar conclusions, studying the luminosity curve of SNe with RSG progenitors.”