Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Deflagration to Detonation Density

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

doi:10.22323/1.100.0251

Cited by 3 publications

(3 citation statements)

References 10 publications

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“…After burning a part of the star, a detonation front is formed that burns the remaining parts. This scenario reproduces the main characteristics of normal SNe Ia [6,3,7,8,9,10] well. Synthetic lightcurves from multidimensional simulations of Chandrasekhar-mass delayed detonations are in good agreement with observations [11].…”

Section: Chandrasekhar-mass Delayed Detonationssupporting

confidence: 70%

Type Ia Supernovae (invited talk)

Pakmor¹,

Fink²,

Hillebrandt³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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The progenitor system and explosion mechanism of Type Ia Supernovae (SNe Ia) is still uncertain, despite the large amount of observational data we have today. Given the importance of SNe Ia for different fields including nucleosynthesis, galactic chemical evolution and cosmology this is clearly unsatisfactory. Here we show results of consistent multidimensional modeling of three different explosion scenarios from the onset of the first thermonuclear flame to synthetic lightcurves and spectra. This way, we can predict the optical display of our models, compare it to observations and ideally identify the actual progenitor system and explosion mechanism. Contrary to previous results, we find that they all show good agreement with observations, so we cannot rule out any of these scenarios just yet, but they are possibly all realized in Nature. In this case, additional information like binary population synthesis will have to be taken into account to determine the dominant scenario among all SNe Ia.

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Section: Chandrasekhar-mass Delayed Detonationssupporting

confidence: 70%

Type Ia Supernovae (invited talk)

Pakmor¹,

Fink²,

Hillebrandt³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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“…Curves with different ∆ e indicate the filter size in units of grid cell widths for the measurement operation. Shown for comparison are curves from our 2D study [10] resulting in the highest yield (r18) and lowest yield (r10) indicating that the green curve shows a similar expansion history to that calculated in 2D.…”

Section: Figurementioning

confidence: 84%

Turbulence-Flame Interaction on the Early Evolution of Flames in Type Ia Supernovae

Calder¹,

Jackson²,

Townsley³

et al. 2011

Proceedings of 11th Symposium on Nuclei in the Cosmos — PoS(NIC XI)

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Type Ia supernovae are bright stellar explosions thought to occur when a runaway thermonuclear reaction incinerates a compact star known as white dwarf (WD). In many models, the explosion begins with a flame born in the turbulent environment near the center of the white dwarf. The effect of turbulence on the evolution of the nascent flame is incompletely understood and is the subject of active research. The range of length scales from the full star (∼ 10 8 cm) to the laminar flame width (∼ 10 −5 cm) prevents full-star simulations from resolving the turbulence-flame interaction (TFI) directly. In the single-degenerate paradigm of Type Ia supernovae (SNe Ia), the WD experiences ∼ 1000 year period of convection as the temperature rises to burn carbon. When the nuclear burning timescale exceeds the turnover time for convective eddies, a flame is born in * Speaker.

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“…The multi-dimensional representation of the ignition configuration (e.g., [34]) allows for a substantial variation in the brightness of the modeled event [35,36,32,33]. Several other parameters, however, may also contribute to the variability [37,38,39,40].…”

Section: Pos(nic Xii)046mentioning

confidence: 99%

Type Ia supernovae: exposing models to observations

Röpke¹,

Fink²,

Hillebrandt

et al. 2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

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Type Ia supernovae play an important role in observational cosmology and in various astrophysical processes. As main producers of iron group elements, they are a key component in the cosmic cycle of matter. The questions about the nature of the progenitor systems from which these cosmic explosions arise and of their physical mechanism, however, are not settled. Several possibilities have been suggested in the literature. We discuss recent developments and present multidimensional explosion simulations referring to two different scenarios. Combined with detailed radiative transfer calculations that predict observables from the models and allow direct comparison with astronomical data, these simulations shed light on the nature of the progenitor systems. Although the range of observed properties is large enough to accommodate many theoretical explosion models, it is particularly important to identify the class of objects that constitutes the bulk of Type Ia supernovae. Even when starting out from systems as diverse as Chandrasekhar-mass white dwarfs and double white dwarf mergers, there is some degeneracy in the predicted observables that prevents a straightforward judgement on the validity of the models. We discuss possible ways to overcome this problem and to discriminate between different scenarios.

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Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Deflagration to Detonation Density

Cited by 3 publications

References 10 publications

Type Ia Supernovae (invited talk)

Type Ia Supernovae (invited talk)

Turbulence-Flame Interaction on the Early Evolution of Flames in Type Ia Supernovae

Type Ia supernovae: exposing models to observations

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