EVALUATING SYSTEMATIC DEPENDENCIES OF TYPE Ia SUPERNOVAE: THE INFLUENCE OF DEFLAGRATION TO DETONATION DENSITY

Jackson, Aaron P.; Calder, A. C.; Townsley, Dean M.; Chamulak, David A.; Brown, Edward F.; Timmes, F. X.

doi:10.1088/0004-637x/720/1/99

Cited by 60 publications

(113 citation statements)

References 57 publications

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“…Although this dependence has already been addressed elsewhere (Bravo et al 2010;Jackson et al 2010), it is somewhat speculative and we prefer not to mix it with the already hypothetical character of our ghost resonance.…”

Section: Physical Conditions At Thermal Runawaymentioning

confidence: 92%

Type Ia supernovae and the¹²C+¹²C reaction rate

Bravo

Piersanti

Domínguez

et al. 2011

A&A

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Context. Even if the 12 C+ 12 C reaction plays a central role in the ignition of type Ia supernovae (SNIa), the experimental determination of its cross-section at astrophysically relevant energies (E 2 MeV) has never been made. The profusion of resonances throughout the measured energy range has led to speculation that there is an unknown resonance at E 0 ∼ 1.5 MeV possibly as strong as the one measured for the resonance at 2.14 MeV, i.e. (ωγ) R = 0.13 meV. Aims. We study the implications that such a resonance would have for our knowledge of the physics of SNIa, paying special attention to the phases that go from the crossing of the ignition curve to the dynamical event.Methods. We use one-dimensional hydrostatic and hydrodynamic codes to follow the evolution of accreting white dwarfs until they grow close to the Chandrasekhar mass and explode as SNIa. In our simulations, we account for a low-energy resonance by exploring the parameter space allowed by experimental data. Results. A change in the 12 C+ 12 C rate similar to the one explored here would have profound consequences for the physical conditions in the SNIa explosion, namely the central density, neutronization, thermal profile, mass of the convective core, location of the runaway hot spot, or time elapsed since crossing the ignition curve. For instance, with the largest resonance strength we use, the time elapsed since crossing the ignition curve to the supernova event is shorter by a factor ten than for models using the standard rate of 12 C+ 12 C, and the runaway temperature is reduced from ∼8.14 × 10 8 K to ∼4.26 × 10 8 K. On the other hand, a resonance at 1.5 MeV, with a strength ten thousand times smaller than the one measured at 2.14 MeV, but with an α/p yield ratio substantially different from 1 would have a sizeable impact on the degree of neutronization of matter during carbon simmering. Conclusions. A robust understanding of the links between SNIa properties and their progenitors will not be attained until the 12 C+ 12 C reaction rate is measured at energies ∼1.5 MeV.

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Section: Physical Conditions At Thermal Runawaymentioning

confidence: 92%

Type Ia supernovae and the¹²C+¹²C reaction rate

Bravo

Piersanti

Domínguez

et al. 2011

A&A

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“…The main model is a 2-dimensional simulation of a Chandrasekhar-mass WD exploding via the deflagration-detonation transition (DDT) mechanism. These simulations are identical to those we have performed previously to study systematic variation in this scenario (Krueger et al 2010;Jackson et al 2010;Krueger et al 2012). For comparison, we also compute nucleosynthetic yields, spectra, and light-curves for the well-studied, 1-dimensional W7 model (Nomoto et al 1984).…”

mentioning

confidence: 97%

On Measuring the Metallicity of a Type Ia Supernova’s Progenitor

Miles

Rossum

Townsley

et al. 2016

ApJ

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In Type Ia Supernovae (SNe Ia), the relative abundances of chemical elements are affected by the neutron excess in the composition of the progenitor white dwarf. Since these products leave signatures in the spectra near maximum light, spectral features may be used to constrain the composition of the progenitor. We calculate the nucleosynthetic yields for three SN Ia simulations, assuming single degenerate, Chandrasekhar mass progenitors, for a wide range of progenitor metallicities, and calculate synthetic light curves and spectra to explore correlations between progenitor metallicity and the strength of spectral features. We use two 2D simulations of the deflagration-detonation-transition scenario with different 56 Ni yields and the W7 simulation to control for differences between explosion models and total yields. While the overall yields of intermediate mass elements (16 < A ≤ 40) differ between the three cases, trends in the yields are similar. With increasing metallicity, 28 Si yields remain nearly constant, 40 Ca yields decline, and Ti and 54 Fe yields increase. In the synthetic spectra, we identify two features at 30 days post explosion that appear to deepen with progenitor metallicity: a Ti feature around 4200Å and a Fe feature around 5200Å. In all three simulations, their pseudo equivalent widths show a systematic trend with progenitor metallicity. This suggests that these two features may allow differentiation among progenitor metallicities of observed SNe Ia and potentially help reduce the intrinsic Hubble scatter.

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“…The paradigm of the delayed detonation models is consistent with the theoretical models [53,54] and with theoretical conclusion [55] that a detonation in a strongly Fermi-degenerated matter is unstable against 1D pulsations at densities higher than 7 3 2 10 g / cm  and it becomes stable at lower densities near the star surface. There has been numerous attempts both analytical and numerical [50][51][52][53][54][55][56][57][58][59][60] During the late deflagration phase the radiant flux produced by the radioactive decays of 56 56 56 Ni Co Fe   increases considerably in course of the star incineration by the expanding deflagration wave. Absorption of the radiant energy flux in the outer layers of the star may produce a preconditioned region with the shallow temperature gradient such that detonation can be ignited via the Zel'dovich gradient mechanism.…”

Section: Discussionmentioning

confidence: 99%

Radiation heat transfer in particle-laden gaseous flame: Flame acceleration and triggering detonation

2015

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In this study we examine influence of the radiation heat transfer on the combustion regimes in the mixture, formed by suspension of fine inert particles in hydrogen gas. The gaseous phase is assumed to be transparent for the thermal radiation, while the radiant heat absorbed by the particles is then lost by conduction to the surrounding gas. The particles and gas ahead of the flame is assumed to be heated by radiation from the original flame. It is shown that the maximum temperature increase due to the radiation preheating becomes larger for a flame with lower velocity. For a flame with small enough velocity temperature of the radiation preheating may exceed the crossover temperature, so that the radiation heat transfer may become a dominant mechanism of the flame propagation. In the case of non-uniform distribution of particles, the temperature gradient formed due to the radiation preheating can initiate either deflagration or detonation ahead of the original flame via the Zel'dovich's gradient mechanism. The initiated combustion regime ignited in the preheat zone ahead of the flame depends on the radiation absorption length and on the steepness of the formed temperature gradient. Scenario of the detonation triggering via the temperature gradient mechanism formed due to the radiation preheating is plausible explanation of the transition to detonation in Supernovae Type Ia explosion.

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EVALUATING SYSTEMATIC DEPENDENCIES OF TYPE Ia SUPERNOVAE: THE INFLUENCE OF DEFLAGRATION TO DETONATION DENSITY

Cited by 60 publications

References 57 publications

Type Ia supernovae and the¹²C+¹²C reaction rate

Type Ia supernovae and the¹²C+¹²C reaction rate

On Measuring the Metallicity of a Type Ia Supernova’s Progenitor

Radiation heat transfer in particle-laden gaseous flame: Flame acceleration and triggering detonation

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EVALUATING SYSTEMATIC DEPENDENCIES OF TYPE Ia SUPERNOVAE: THE INFLUENCE OF DEFLAGRATION TO DETONATION DENSITY

Cited by 60 publications

References 57 publications

Type Ia supernovae and the12C+12C reaction rate

Type Ia supernovae and the12C+12C reaction rate

On Measuring the Metallicity of a Type Ia Supernova’s Progenitor

Radiation heat transfer in particle-laden gaseous flame: Flame acceleration and triggering detonation

Contact Info

Product

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Type Ia supernovae and the¹²C+¹²C reaction rate

Type Ia supernovae and the¹²C+¹²C reaction rate