Theoretical light curves for deflagration models of Type Ia supernova

By S. Blinnikov, F. Roepke, E. Sorokina, M. Gieseler, M. Reinecke, C. Travaglio, W. Hillebrandt, M. Mpa, Garching, Itep and 6 more. 2006

221 citations recorded by the source corpus.

Aims. We present synthetic bolometric and broad-band UBVRI light curves of SNe Ia for four selected 3D deflagration models of thermonuclear supernovae. Methods. The light curves are computed with the 1D hydro code stella, which models (multi-group time-dependent) nonequilibrium radiative transfer inside SN ejecta. Angle-averaged results from 3D hydrodynamical explosion simulations with the composition determined in a nucleosynthetic postprocessing step served as the input to the radiative transfer model. Results. The predicted model UBV light curves do agree reasonably well with the observed ones for SNe Ia in the range of low to normal luminosities, although the underlying hydrodynamical explosion models produced only a modest amount of radioactive 56 Ni (i.e. ∼0.24–0.42 M� ) and relatively low kinetic energy in the explosion (less than 0.7 × 10 51 erg). The evolution of predicted B and ∞

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d2cfdca7855c200a8213d484509bc425cd839349

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Citations in the corpus

• Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, background): “STELLA is a one-dimensional multigroup radiation hydrodynamics code (Blinnikov & Bartunov 1993; Blinnikov et al. 1998, 2006; Blinnikov & Tolstov 2011) and calculates the spectral energy distributions (SEDs) at each time step.”
• Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions (2017, methodology): “…hydrodynamics, Rayleigh–Taylor instability modeling in 1D (Duffell 2016), and radiative transfer using the public version of the STELLA instrument (Blinnikov & Sorokina 2004; Baklanov et al. 2005; Blinnikov et al. 2006)—open up new avenues for researching the diverse set of TypeII supernovae.”
• Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “…the light curves generated by SNEC and the multigroup radiation-hydrodynamic code STELLA (Blinnikov & Bartunov 1993, 2011; Baklanov et al. 2005; Blinnikov et al. 2006; Kozyreva et al. 2017) that uses the same RSG progenitor shows good agreement in the bolometric luminosity and plateau duration…”
• 3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae (2012, background): “The models presented by Blinnikov et al. (2006), however, do not allow for a detailed comparison to the observed spectral time sequence since the multi-group approximation employed in their radiative transfer simulations is too coarse.”
• Supernovae from red supergiants with extensive mass loss (2010, methodology): “For the details of STELLA, see Blinnikov et al. (2006) and the references therein.”
• Time-dependent three-dimensional spectrum synthesis for Type Ia supernovae (2009, methodology): “We start with the light curves from the multi-energy group radiation hydrodynamics code stella (Blinnikov et al. 2006) which treats the line opacity in the expansion opacity formalism (Karp et al. 1977; Friend & Castor 1983; Eastman & Pinto 1993).”
• Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, methodology): “…include the deterministic code PHOENIX (van Rossum 2012) for the W7 model of Type Ia supernovae (SN Ia) (Wollaeger & van Rossum 2014), and the codes STELLA (Blinnikov et al. 2006), RHMC (Noebauer et al. 2012), and V1D (Livne 1993) for a grey pair-instability supernova model (Kozyreva et al. 2017).”
• The 511 keV emission from positron annihilation in the Galaxy (2010, background): “However, 3D effects may considerably alter the stratification of radioactivities inside the SNIa (Blinnikov et al., 2006), allowing for substantial amounts of 56Ni to be mixed out to the surface (Fig.”
• GENERALIZED SEMI-ANALYTICAL MODELS OF SUPERNOVA LIGHT CURVES (2011, methodology): “D radiation hydrodynamics code STELLA (Blinnikov & Bartunov 1993; Blinnikov et al. 1998; Blinnikov et al. 2006) reproduced the LC of ultraviolet-rich SN IIP SN 2009kf reasonably well and provided a tool to study the LCs of low-luminosity SN IIn powered by the interaction of the SN ejecta with a CS…”
• The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations? (2006, methodology): “…models—ones in which the nuclear burning front remains subsonic throughout the entire explosion—do not produce sufficient 56Ni and kinetic energy, are too mixed, and leave behind too much unburned carbon and oxygen to account for normalluminosity SNe Ia (Gamezo et al. 2004; Blinnikov et al. 2006).”