Time-dependent three-dimensional spectrum synthesis for Type Ia supernovae

By M. Kromer, Stuart A. Sim. 2009

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A Monte Carlo code (artis) for modelling time-dependent three-dimensional spectral synthesis in chemically inhomogeneous models of Type Ia supernova ejecta is presented. Following the propagation of γ-ray photons, emitted by the radioactive decay of the nucleosynthesis products, energy is deposited in the supernova ejecta and the radiative transfer problem is solved self-consistently, enforcing the constraint of energy conservation in the comoving frame. Assuming a photoionization-dominated plasma, the equations of ionization equilibrium are solved together with the thermal balance equation adopting an approximate treatment of excitation. Since we implement a fully general treatment of line formation, there are no free parameters to adjust. Thus, a direct comparison between synthetic spectra and light curves, calculated from hydrodynamic explosion models, and observations is feasible. The code is applied to the well-known W7 explosion model and the results tested against other studies. Finally, the effect of asymmetric ejecta on broad-band light curves and spectra is illustrated using an elliptical toy model.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fb4130c75d79b67868093a6ab1613828a2bbc060

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Citations in the corpus

Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “Thus, unlike the typical Sobolev expansion opacity formalism in Monte Carlo codes (see, for instance, Kasen et al. (2006); Kromer & Sim (2009)), line transfer is not directly treated by SuperNu.”
CONSTRAINING TYPE Ia SUPERNOVA MODELS: SN 2011fe AS A TEST CASE (2012, methodology): “To this end, we simulated the propagation of 108 photon packets from 2 to 120 days after explosion using the cd23 gf-5 atomic dataset of Kromer & Sim (2009), which is based on the lines contained in the CD23 compilation of Kurucz & Bell (1995).”
NORMAL TYPE Ia SUPERNOVAE FROM VIOLENT MERGERS OF WHITE DWARF BINARIES (2012, methodology): “Here, however, we have restricted ourselves for computational reasons to a simplified atomic data set (cd23_gf5 of Kromer & Sim 2009) with only∼ 400,000 lines.”
Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae (2013, methodology): “To reduce the computational costs, a grey approximation is used in optically thick cells (cf. Kromer & Sim 2009) and for t < 3 d, local thermodynamic equilibrium is assumed.”
3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae (2012, methodology): “To speed up the initial phase, a grey approximation, as discussed by Kromer & Sim (2009), was used in optically thick cells, and the initial 10 time steps (i.e. the initial three days after the explosion) were treated in local thermodynamic equilibrium (LTE).”
Double-detonation sub-Chandrasekhar supernovae: can minimum helium shell masses detonate the core? (2010, methodology): “8 we show angle-averaged ultraviolet-optical-infrared (UVOIR) light curves for all six of our models (computed with the artis code; Kromer & Sim 2009; Sim 2007; corresponding values are given in Table 4).”
Sub-Chandrasekhar-mass White Dwarf Detonations Revisited (2017, background): “As noted by Kromer & Sim (2009) and Sim et al. (2010), different radiative transfer codes produce somewhat different light curves for the same input; further work is necessary to ascertain the cause of the mismatch.”
RADIATIVE TRANSFER SIMULATIONS OF NEUTRON STAR MERGER EJECTA (2013, methodology): “Kromer & Sim (2009) demonstrated that the number of bound–bound transitions included in the simulation mostly affects the NIR light curves (black and gray lines in Figure 13).”
DOUBLE-DETONATION SUB-CHANDRASEKHAR SUPERNOVAE: SYNTHETIC OBSERVABLES FOR MINIMUM HELIUM SHELL MASS MODELS (2010, methodology): “Here, however, we have restricted ourselves for computational reasons to a simplified atomic data set (cd23_gf-5 of Kromer & Sim 2009) with only ∼400,000 lines.”
The 44Ti-powered spectrum of SN 1987A (2011, methodology): “Applications and further developments of this method are described in e.g. Sim (2007), Sim et al. (2007) and Kromer & Sim (2009).”
High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, background): “Since the majority of the flux in the NIR is caused by fluorescence (e.g. Kromer & Sim 2009), the lack of emission compared to ordinary SNe Ia around the time of B-band maximum suggests less flux C© 2011 The Authors, MNRAS 412, 2735–2762 Monthly Notices of the Royal Astronomical Society C© 2011…”
DETONATIONS IN SUB-CHANDRASEKHAR-MASS C+O WHITE DWARFS (2010, methodology): “For example, applying different radiative transfer codes to the well-known W7 model (Nomoto et al. 1984; Thielemann et al. 1986), which is widely regarded as a good standard for normal SNe Ia, yields∆m15-values that differ by several tenths of a magnitude (see e.g. figure 7 of Kromer & Sim 2009).”