Abstract
Abstract Type II-plateau supernovae (SNe IIP) are the most numerous subclass of core-collapse SNe originating from massive stars. In the framework of the neutrino-driven explosion mechanism, we study the properties of the SN outburst for a red supergiant progenitor model and compare the corresponding light curves with observations of the ordinary Type IIP SN 1999em. Three-dimensional (3D) simulations of (parametrically triggered) neutrino-driven explosions are performed with the (explicit, finite-volume, Eulerian, multifluid hydrodynamics) code Prometheus, using a presupernova model of a 15 M ⊙ star as initial data. On approaching homologous expansion, the hydrodynamic and composition variables of the 3D models are mapped to a spherically symmetric configuration, and the simulations are continued with the (implicit, Lagrangian, radiation hydrodynamics) code Crab to follow the evolution of the blast wave during the SN outburst. Our 3D neutrino-driven explosion model with an explosion energy of about erg produces 56Ni in rough agreement with the amount deduced from fitting the radioactively powered light-curve tail of SN 1999em. The considered presupernova model, 3D explosion simulations, and light-curve calculations can explain the basic observational features of SN 1999em, except for those connected to the presupernova structure of the outer stellar layers. Our 3D simulations show that the distribution of 56Ni-rich matter in velocity space is asymmetric with a strong dipole component that is consistent with the observations of SN 1999em. The monotonic decline in luminosity from the plateau to the radioactive tail in ordinary SNe IIP is a manifestation of the intense turbulent mixing at the He/H composition interface.
Highlights
Massive stars in the range of ∼9−25...30 M produce a core of iron which collapses to a neutron star with the subsequent explosion ending the stellar lives as type II-plateau supernovae (SNe IIP) (e.g., Heger et al 2003)
Relative fractions of the ordinary SNe IIP and the SN 1987A-like events are about 50% (Li et al 2011; Smith et al 2011) and 1–3% (Pastorello et al 2012) of all corecollapse SNe (CCSNe), respectively. It is theoretically established (Grassberg et al 1971; Falk & Arnett 1977) and empirically confirmed (Smartt 2009) that the most common ordinary SNe IIP originate from red supergiant (RSG) stars, while the peculiar objects are identified with the explosions of blue supergiant (BSG) stars (e.g., Arnett et al 1989)
The present paper is our second attempt to model the light curves of type IIP supernova explosions based on 3D explosion models (our first one was concerned with the peculiar type IIP SN 1987A Utrobin et al (2015))
Summary
Massive stars in the range of ∼9−25...30 M produce a core of iron which collapses to a neutron star with the subsequent explosion ending the stellar lives as type II-plateau supernovae (SNe IIP) (e.g., Heger et al 2003). Ordinary SNe IIP exhibit a wide range of luminosities in the plateau phase and total masses of radioactive 56Ni, which is illustrated, for example, by the luminous SN 2004et, the normal SN 1999em, and the sub-luminous SN 2012A (Fig. 1) All of these SNe originate from RSG stars, and their luminosities are produced by the release of the internal energy deposited during the shock wave propagation through the pre-SN envelope. As in the case of SN 1987A (Utrobin et al 2015), we carry out 3D hydrodynamic simulations of neutrino-driven explosions for the evolutionary preSN model of an RSG star These simulations yield a complex morphology of radioactive 56Ni and hydrogen mixing. The pre-SN model, which we name L15, provides the initial data for our 3D neutrino-driven CCSN explosion simulations It has a helium core of 4.35 M and a radius of 627 R typical of RSG stars (Table 1, Fig. 2). Both in model L15-pn and the optimal model, which are exploded with a 1D piston, 56Ni is mixed artificially and nearly uniformly in velocity space up to ≈450 and 660 km s−1, respectively
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