The influence of chemical composition on models of Type Ia supernovae

Calder, A. C.; Krueger, Brendan K.; Jackson, Aaron P.; Townsley, Dean M.

doi:10.1007/s11467-013-0301-4

Cited by 23 publications

(17 citation statements)

References 234 publications

(394 reference statements)

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“…A detailed account of SN Ia models is beyond the scope of our general review of SN Ia spectra (for the latest discussions, see Wang and Han 2012;Nomoto et al 2013;Hillebrandt et al 2013;Calder et al 2013;Maoz et al 2013). However, in order to understand the context by which observations are taken and synthetic comparisons made, here we only mention the surface layer of matters relating to observed spectra.…”

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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Section: Modelsmentioning

confidence: 99%

A review of type Ia supernova spectra

Parrent

Friesen

Parthasarathy

2014

Astrophys Space Sci

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“…In the previous studies of the susy model cited above, there was no consideration of the supernova-host-galaxy correlations which are taken up in the present article. In the binary models, the host-galaxy effects could be related to effects on the rate of mass growth although chemical composition effects in binary models have also been proposed [8]. Some of the predictions of this latter study are, however, not in full agreement with data.…”

Section: Introductionmentioning

confidence: 73%

“…Since iron is inert to fusion, the expression eq. 2.1 nevertheless highlights the expectation that, if fusion is the sole energy source, the nickel production and supernova energy release decrease with heavy element abundance contrary to empirical indications (See, for example, figure 2 of [8]).…”

Section: The White Dwarf Mass Distributionmentioning

confidence: 86%

Host galaxy effects in the SUSY model for Supernovae Ia

Clavelli

2018

Int. J. Mod. Phys. A

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For more than forty years virtually all work on the theory of type Ia Supernovae (SN Ia) has assumed that these explosions were due to the transfer of mass to a degenerate star from a partner in a binary system. In these binary models, when the mass of one partner closely approaches the Chandrasekhar maximum for a stable degenerate system, fusion can be initiated and the star explodes. However, a number of long-standing nagging problems and the inability of any specific binary model to fit any significant fraction of SN Ia events suggest that fusion could instead be triggered by a phase transition in a sub-Chandrasekhar white dwarf star. It is possible that remarkable host galaxy effects not considered in previous work on phase transition models could point to a specific source of the supernova trigger. Performing a least χ 2 fit to the delay time distribution to fix parameters, we give predictions from the susy phase transition model for the host galaxy effects. In addition we discuss a susy insight into the Phillips relation which is basic to the cosmological importance of the type Ia supernovae.

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“…For sub-M Ch scenarios, the settling of the 22 Ne within the WD (Bildsten and Hall, 2001) may be important for the distribution of stable IGE in the ejecta. Metallicity can also change the explosion in other ways (Calder et al, 2013) including modification of the DDT density (Jackson et al, 2010).…”

Section: Explosive Thermonuclear Burningmentioning

confidence: 99%

Nucleosynthesis in Thermonuclear Supernovae

Seitenzahl¹,

Townsley²

2017

Handbook of Supernovae

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The explosion energy of thermonuclear (Type Ia) supernovae is derived from the difference in nuclear binding energy liberated in the explosive fusion of light "fuel" nuclei, predominantly carbon and oxygen, into more tightly bound nuclear "ash" dominated by iron and silicon group elements. The very same explosive thermonuclear fusion event is also one of the major processes contributing to the nucleosynthesis of the heavy elements, in particular the iron-group elements. For example, most of the iron and manganese in the Sun and its planetary system was produced in thermonuclear supernovae. Here, we review the physics of explosive thermonuclear burning in carbon-oxygen white dwarf material and the methodologies utilized in calculating predicted nucleosynthesis from hydrodynamic explosion models. While the dominant explosion scenario remains unclear, many aspects of the nuclear combustion and nucleosynthesis are common to all models and must occur in some form in order to produce the observed yields. We summarize the predicted nucleosynthetic yields for existing explosions models, placing particular emphasis on characteristic differences in the nucleosynthetic signatures of the different suggested scenarios leading to Type Ia supernovae. Following this, we discuss how these signatures compare with observations of several individual supernovae, remnants, and the composition of material in our Galaxy and galaxy clusters.

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The influence of chemical composition on models of Type Ia supernovae

Cited by 23 publications

References 234 publications

A review of type Ia supernova spectra

A review of type Ia supernova spectra

Host galaxy effects in the SUSY model for Supernovae Ia

Nucleosynthesis in Thermonuclear Supernovae

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