Detailed Spectral Modeling of a Three‐dimensional Pulsating Reverse Detonation Model: Too Much Nickel

Baron, Edward; Jeffery, David J.; Branch, David; Bravo, Eduardo; Garcı́a-Senz, Domingo; Hauschildt, P. H.

doi:10.1086/524009

Cited by 19 publications

(24 citation statements)

References 54 publications

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“…The composition profile in the GCD model is therefore significantly different from that in the pulsational reverse detonation (PRD) model described by Bravo & García-Senz (2006) and discussed in Baron et al (2008). The total mass of Fe-peak material in the outer layers is significantly smaller in the GCD model, residing within a thin surface layer overlying a region rich in IMEs.…”

Section: The Velocity Distribution Of the Yieldmentioning

confidence: 72%

STUDY OF THE DETONATION PHASE IN THE GRAVITATIONALLY CONFINED DETONATION MODEL OF TYPE Ia SUPERNOVAE

Meakin

Seitenzahl

Townsley

et al. 2009

ApJ

100

118

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We study the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia) through the detonation phase and into homologous expansion. In the GCD model, a detonation is triggered by the surface flow due to single-point, off-center flame ignition in carbon-oxygen white dwarfs (WDs). The simulations are unique in terms of the degree to which nonidealized physics is used to treat the reactive flow, including weak reaction rates and a time-dependent treatment of material in nuclear statistical equilibrium (NSE). Careful attention is paid to accurately calculating the final composition of material which is burned to NSE and frozen out in the rapid expansion following the passage of a detonation wave over the high-density core of the WD; and an efficient method for nucleosynthesis postprocessing is developed which obviates the need for costly network calculations along tracer particle thermodynamic trajectories. Observational diagnostics are presented for the explosion models, including abundance stratifications and integrated yields. We find that for all of the ignition conditions studied here a self-regulating process comprised of neutronization and stellar expansion results in final 56 Ni masses of ∼1.1 M . But, more energetic models result in larger total NSE and stable Fe-peak yields. The total yield of intermediate mass elements is ∼ 0.1 M and the explosion energies are all around 1.5 × 10 51 erg. The explosion models are briefly compared to the inferred properties of recent SN Ia observations. The potential for surface detonation models to produce lower-luminosity (lower 56 Ni mass) SNe is discussed.

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Section: The Velocity Distribution Of the Yieldmentioning

confidence: 72%

STUDY OF THE DETONATION PHASE IN THE GRAVITATIONALLY CONFINED DETONATION MODEL OF TYPE Ia SUPERNOVAE

Meakin

Seitenzahl

Townsley

et al. 2009

ApJ

100

118

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“…At the same time, the observed characteristics of SN Ia light curves and spectra can be fairly matched by adopting radial and/or axial shifts in the distribution of 56 Ni, possibly due to a delayed-and/or pulsational-detonation-like explosion mechanism (see Khokhlov 1991b;Hoflich et al 1995;Baron et al 2008Baron et al , 2012Bravo et al 2009;Maeda et al 2010b;Dessart et al 2013a) or a merger scenario (e.g., Dan et al 2013;Moll et al 2013). Central ignition densities are also expected to play a secondary role in the form of the WLR since they are dependent upon the accretion rate of H and/or He-rich material and cooling time Höflich et al 2010;Meng et al 2010;Krueger et al 2010;Sim et al 2013), in addition to the spin-down timescales for differentially rotating WDs (Hachisu et al 2012;Tornambé and Piersanti 2013).…”

Section: Light Curvesmentioning

confidence: 85%

“…To their advantage, these deflagrationto-detonation transition (DDT) and pulsating delayed-detonation (PDD) models are able to reproduce the observed characteristics of SN Ia, however not without the use of an artificially-set transition density between stages of burning (Khokhlov 1991b;Hoflich et al 1995;Lentz et al 2001aLentz et al , 2001bBaron et al 2008;Bravo et al 2009;Dessart et al 2013a). Subsequently, a bulk of the efforts within the modeling community has been the pursuit of conditions or mechanisms which cause the burning front to naturally transition from a sub-sonic deflagration to a super-sonic detonation, e.g., gravitationally confined detonations (Jordan et al 2009), prompt detonations of merging WDs, a.k.a.…”

Section: Modelsmentioning

confidence: 99%

A review of type Ia supernova spectra

Parrent

Friesen

Parthasarathy

2014

Astrophys Space Sci

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SN 2011fe was the nearest and best-observed type Ia supernova in a generation, and brought previous incomplete datasets into sharp contrast with the detailed new data. In retrospect, documenting spectroscopic behaviors of type Ia supernovae has been more often limited by sparse and incomplete temporal sampling than by consequences of signal-to-noise ratios, telluric features, or small sample sizes. As a result, type Ia supernovae have been primarily studied insofar as parameters discretized by relative epochs and incomplete temporal snapshots near maximum light. Here we discuss a necessary next step toward consistently modeling and directly measuring spectroscopic observables of type Ia supernova spectra. In addition, we analyze current spectroscopic data in the parameter space defined by empirical metrics, which will be relevant even after progenitors are observed and detailed models are refined.

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“…Models GCD1 and TURB7 synthesize a large amount of 56 Ni and, due to their large kinetic energy and the presence of radioactive nuclei up to the surface of the ejecta, decline much faster than observations seem to indicate (the main parameter determining the width of the bolometric light curve is the photon diffusion time, t d , that is in turn affected by the kinetic energy: t d ∝ K −1/4 , Woosley et al 2007). Baron et al (2008) obtained detailed spectra of angle-averaged one-dimensional versions of several PRD models, from slightly before up to a few days after maximum light. They concluded that the synthetic spectra of the PRD models did not match the spectra of a few typical wellobserved SNIa.…”

Section: Light Curvesmentioning

confidence: 99%

PULSATING REVERSE DETONATION MODELS OF TYPE Ia SUPERNOVAE. II. EXPLOSION

Bravo

Garcı́a-Senz

Cabezón

et al. 2009

ApJ

Self Cite

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Observational evidences point to a common explosion mechanism of Type Ia supernovae based on a delayed detonation of a white dwarf. However, all attempts to find a convincing ignition mechanism based on a delayed detonation in a destabilized, expanding, white dwarf have been elusive so far. One of the possibilities that has been invoked is that an inefficient deflagration leads to pulsation of a Chandrasekhar-mass white dwarf, followed by formation of an accretion shock that confines a carbon-oxygen rich core, while transforming the kinetic energy of the collapsing halo into thermal energy of the core, until an inward moving detonation is formed. This chain of events has been termed Pulsating Reverse Detonation (PRD). In this work we present three dimensional numerical simulations of PRD models from the time of detonation initiation up to homologous expansion. Different models characterized by the amount of mass burned during the deflagration phase, M defl , give explosions spanning a range of kinetic energies, K ∼ (1.0 − 1.2) × 10 51 erg, and 56 Ni masses, M ( 56 Ni) ∼ 0.6 − 0.8 M ⊙ , which are compatible with what is expected for typical Type Ia supernovae. Spectra and light curves of angle-averaged spherically symmetric versions of the PRD models are discussed. Type Ia supernova spectra pose the most stringent requirements on PRD models.

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Detailed Spectral Modeling of a Three‐dimensional Pulsating Reverse Detonation Model: Too Much Nickel

Cited by 19 publications

References 54 publications

STUDY OF THE DETONATION PHASE IN THE GRAVITATIONALLY CONFINED DETONATION MODEL OF TYPE Ia SUPERNOVAE

STUDY OF THE DETONATION PHASE IN THE GRAVITATIONALLY CONFINED DETONATION MODEL OF TYPE Ia SUPERNOVAE

A review of type Ia supernova spectra

PULSATING REVERSE DETONATION MODELS OF TYPE Ia SUPERNOVAE. II. EXPLOSION

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