THE DETONATION MECHANISM OF THE PULSATIONALLY ASSISTED GRAVITATIONALLY CONFINED DETONATION MODEL OF Type Ia SUPERNOVAE

Jordan, G. C.; Graziani, C.; Fisher, Robert; Townsley, Dean M.; Meakin, Casey; Weide, Klaus; Reid, Lynn B.; Norris, John M.; Hudson, Randy; Lamb, D. Q.

doi:10.1088/0004-637x/759/1/53

Cited by 54 publications

(45 citation statements)

References 60 publications

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“…Since the spatial scales relevant to the initiation of a detonation cannot be resolved in full-star multi-dimensional explosion simulations (see the discussion in Seitenzahl et al 2009a), it is common practice (e.g. Jordan et al 2008Jordan et al , 2012aGuillochon et al 2010;Pakmor et al 2011Pakmor et al , 2012b to pick a certain critical density ρ crit and temperature T crit that a cell composed of nuclear fuel must exceed for a detonation to be initiated. However, these critical values are no more than informed guesses based on separate high-resolution onedimensional detonation initiation calculations (e.g.…”

Section: Hydrodynamic Explosion Simulationsmentioning

confidence: 99%

“…Although successful explosions of near-M Ch WDs in the GCD-framework have been obtained in several hydrodynamical explosion simulations (Plewa 2007;Meakin et al 2009;Jordan et al 2012a), only Meakin et al (2009) have presented detailed isotopic yields for their 2D models. Kasen & Plewa (2007) presented broadband optical and near-infrared light curves, spectral time series, and spectropolarisation for their Y12 model and were generally successful in reproducing the basic properties of observed SNe Ia.…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Seitenzahl

Kromer

Ohlmann

et al. 2016

A&A

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The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae in the single-degenerate evolution channel. It starts with ignition of a deflagration in a single off-centre bubble in a near-Chandrasekharmass white dwarf. Driven by buoyancy, the deflagration flame rises in a narrow cone towards the surface. For the most part, the main component of the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This causes the deflagration ashes to converge again at the opposite side, where the compression heats fuel and a detonation may be launched. We first performed five three-dimensional hydrodynamic simulations of the deflagration phase in 1.4 M carbon/oxygen white dwarfs at intermediate-resolution (256 3 computational zones). We confirm that the closer the initial deflagration is ignited to the centre, the slower the buoyant rise and the longer the deflagration ashes takes to break out and close in on the opposite pole to collide. To test the GCD explosion model, we then performed a high-resolution (512 3 computational zones) simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This high-resolution simulation met our deliberately optimistic detonation criteria, and we initiated a detonation. The detonation burned through the white dwarf and led to its complete disruption. For this model, we determined detailed nucleosynthetic yields by post-processing 10 6 tracer particles with a 384 nuclide reaction network, and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in ultraviolet and blue wavelength bands, which contradicts observed SNe Ia. The strong dependence on the viewing angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we compared our model to SN 1991T. The overall flux level of the model is slightly too low, and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong. Furthermore, the model chemical abundance stratification qualitatively disagrees with recent abundance tomography results in two key areas: our model lacks low-velocity stable Fe and instead has copious amounts of high-velocity 56 Ni and stable Fe. We therefore do not find good agreement of the model with SN 1991T.

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Section: Hydrodynamic Explosion Simulationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Seitenzahl

Kromer

Ohlmann

et al. 2016

A&A

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“…Bravo & García-Senz 2009), and variants of gravitational confined detonation models (e.g. Plewa 2007;Meakin et al 2009;Jordan et al 2012a). In the doubledegenerate scenario (DDS) first proposed by Iben & Tutukov (1984) and Webbink (1984), the progenitor system is a binary system of two WDs.…”

Section: Introductionmentioning

confidence: 99%

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

Seitenzahl

Cescutti

Röpke

et al. 2013

A&A

162

194

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Context. Manganese is predominantly synthesised in Type Ia supernova (SN Ia) explosions. Owing to the entropy dependence of the Mn yield in explosive thermonuclear burning, SNe Ia involving near Chandrasekhar-mass (M Ch ) white dwarfs (WDs) are predicted to produce Mn-to-Fe ratios that significantly exceed those of SN Ia explosions involving sub-Chandrasekhar mass primary WDs. Of all current supernova explosion models, only SN Ia models involving near-M Ch WDs produce [Mn/Fe] 0.0. Aims. Using the specific yields for competing SN Ia scenarios, we aim to constrain the relative fractions of exploding near-M Ch to sub-M Ch primary WDs in the Galaxy. Methods. We extract the Mn yields from three-dimensional thermonuclear supernova simulations that refer to different initial setups and progenitor channels. We then compute the chemical evolution of Mn in the solar neighborhood, assuming SNe Ia are made up of different relative fractions of the considered explosion models. Results. We find that due to the entropy dependence of freeze-out yields from nuclear statistical equilibrium, [Mn/Fe]

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“…Interestingly, for the subclass of SN 2002cx-like SNe, pure deflagrations of Chandrasekhar-mass (Chandrasekhar 1931) WDs (Jordan et al 2012b;Kromer et al 2013;Fink et al 2014) in the SD channel match observables quite well . For normal SNe Ia, the most promising candidates are delayed detonations of Chandrasekhar-mass WDs in SD systems (e.g., Golombek & Niemeyer 2005;Gamezo et al 2005;Röpke & Niemeyer 2007;Bravo & García-Senz 2008;Jordan et al 2008;Townsley et al 2009;Jackson et al 2010;Seitenzahl et al 2011;Röpke et al 2012;Jordan et al 2012a;Seitenzahl et al 2013;Sim et al 2013), double detonations of sub-Chandrasekhar-mass WDs in SD and DD systems (e.g., Fink et al 2007Fink et al , 2010Moll & Woosley 2013), and violent mergers of sub-Chandrasekhar-mass WDs in DD systems (e.g., Pakmor et al 2012aPakmor et al ,b, 2013Moll et al 2014;Raskin et al 2014). A recent comparison to SN 2011fe (Röpke et al 2012) shows that disentangling different models is hard given the current predictions in the optical regime.…”

Section: Introductionmentioning

confidence: 99%

“…Hence, a deflagration flame first burns from the core outwards to the surface, thereby expanding the WD before the detonation is initiated. The mechanism of igniting the detonation is unclear, but several possibilities are proposed and explored in 3D simulations: the spontaneous deflagration-to-detonation transition (spontaneous DDT, Gamezo et al 2005;Röpke & Niemeyer 2007;Bravo & García-Senz 2008;Townsley et al 2009;Jackson et al 2010;Seitenzahl et al 2011;Röpke et al 2012;Seitenzahl et al 2013;Sim et al 2013), the gravitationally confined detonation (GCD, Jordan et al 2008Jordan et al , 2012a, and the pulsational reverse detonation (PRD, ). These models differ in the way the detonation is initiated.…”

Section: Introductionmentioning

confidence: 99%

The white dwarf’s carbon fraction as a secondary parameter of Type Ia supernovae

Ohlmann

Kromer

Fink

et al. 2014

A&A

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Context. Binary stellar evolution calculations predict that Chandrasekhar-mass carbon/oxygen white dwarfs (WDs) show a radially varying profile for the composition with a carbon depleted core. Many recent multi-dimensional simulations of Type Ia supernovae (SNe Ia), however, assume the progenitor WD has a homogeneous chemical composition. Aims. In this work, we explore the impact of different initial carbon profiles of the progenitor WD on the explosion phase and on synthetic observables in the Chandrasekhar-mass delayed detonation model. Spectra and light curves are compared to observations to judge the validity of the model. Methods. The explosion phase is simulated using the finite volume supernova code L, which is extended to treat different compositions of the progenitor WD. The synthetic observables are computed with the Monte Carlo radiative transfer code A. Results. Differences in binding energies of carbon and oxygen lead to a lower nuclear energy release for carbon depleted material; thus, the burning fronts that develop are weaker and the total nuclear energy release is smaller. For otherwise identical conditions, carbon depleted models produce less 56 Ni. Comparing different models with similar 56 Ni yields shows lower kinetic energies in the ejecta for carbon depleted models, but only small differences in velocity distributions and line velocities in spectra. The light curve width-luminosity relation (WLR) obtained for models with differing carbon depletion is roughly perpendicular to the observed WLR, hence the carbon mass fraction is probably only a secondary parameter in the family of SNe Ia.

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THE DETONATION MECHANISM OF THE PULSATIONALLY ASSISTED GRAVITATIONALLY CONFINED DETONATION MODEL OF Type Ia SUPERNOVAE

Cited by 54 publications

References 60 publications

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

The white dwarf’s carbon fraction as a secondary parameter of Type Ia supernovae

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