Constraining the Single-degenerate Channel of Type Ia Supernovae with Stable Iron-group Elements in SNR 3C 397

Dave, Pranav; Kashyap, R.; Fisher, Robert; Timmes, F. X.; Townsley, Dean M.; Byrohl, Chris

doi:10.3847/1538-4357/aa7134

Cited by 33 publications

(43 citation statements)

References 175 publications

(263 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The mechanism underlying the initiation of detonation plays an important role in SNe Ia theory, and much effort has focused upon whether the detonation mechanism in a near-M Ch SD scenario is a DDT or GCD (Röpke et al 2007b;Seitenzahl et al 2016;Dave et al 2017). For example, because the DDT detonates prior to bubble breakout, the stratification of the 56 Ni and IGEs is generally more centrally condensed, in broader agreement with observations of high M Ni56 , overluminous SNe Ia like 91T (Seitenzahl et al 2016).…”

Section: Discussionmentioning

confidence: 57%

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

Byrohl

Fisher

Townsley

2019

ApJ

Self Cite

View full text Add to dashboard Cite

Binary Chandrasekhar-mass white dwarfs accreting mass from non-degenerate stellar companions through the single-degenerate channel have reigned for decades as the leading explanation of Type Ia supernovae. Yet, a comprehensive theoretical explanation has not yet emerged to explain the expected properties of the canonical near-Chandrasekhar-mass white dwarf model. A simmering phase within the convective core of the white dwarf leads to the ignition of one or more flame bubbles scattered across the core. Consequently, near-Chandrasekhar-mass single-degenerate SNe Ia are inherently stochastic, and are expected to lead to a range of outcomes, from subluminous SN 2002cx-like events, to overluminous SN 1991T-like events. However, all prior simulations of the single-degenerate channel carried through the detonation phase have set the ignition points as free parameters. In this work, for the first time, we place ignition points as predicted by ab initio models of the convective phase leading up to ignition, and follow through the detonation phase in fully three-dimensional simulations. Single-degenerates in this framework are characteristically overluminous. Using a statistical approach, we determine the 56 Ni mass distribution arising from stochastic ignition. While there is a total spread of 0.2M for detonating models, the distribution is strongly left-skewed, and with a narrow standard deviation of 0.03M . Conversely, if single-degenerates are not overluminous but primarily yield normal or failed events, then the models require fine-tuning of the ignition parameters, or otherwise require revised physics or progenitor models. We discuss implications of our findings for the modeling of single-degenerate SNe Ia.

show abstract

Section: Discussionmentioning

confidence: 57%

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

Byrohl

Fisher

Townsley

2019

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Its central density at thermal runaway, ρ c = 3×10 9 g cm −3 , is that suggested by some recent studies of the carbon simmering phase (Martínez-Rodríguez et al 2016;Piersanti et al 2017). A central density as high as ρ c = 5 × 10 9 g cm −3 , or even higher, has been invoked to explain the composition of particular SNIa events (Dave et al 2017), while a value as low as ρ c = 2 × 10 9 g cm −3 provides the best nucleosynthetic match with the Solar System ratios of the IGN (Brachwitz et al 2000;Mori et al 2016).…”

Section: Explosion Modelsmentioning

confidence: 65%

Sensitivity of Type Ia supernovae to electron capture rates

Bravo

2019

A&A

View full text Add to dashboard Cite

The thermonuclear explosion of massive white dwarfs is believed to explain at least a fraction of Type Ia supernovae (SNIa). After thermal runaway, electron captures on the ashes left behind by the burning front determine a loss of pressure, which impacts the dynamics of the explosion and the neutron excess of matter. Indeed, overproduction of neutron-rich species such as 54 Cr has been deemed a problem of Chandrasekhar-mass models of SNIa for a long time. I present the results of a sensitivity study of SNIa models to the rates of weak interactions, which have been incorporated directly into the hydrodynamic explosion code. The weak rates have been scaled up/down by a factor ten, either globally for a common bibliographical source, or individually for selected isotopes. In line with previous works, the impact of weak rates uncertainties on sub-Chandrasekhar models of SNIa is almost negligible. The impact on the dynamics of Chandrasekhar-mass models and on the yield of 56 Ni is also scarce. The strongest effect is found on the nucleosynthesis of neutron-rich nuclei, such as 48 Ca, 54 Cr, 58 Fe, and 64 Ni. The species with the highest influence on nucleosynthesis do not coincide with the isotopes that contribute most to the neutronization of matter. Among the last ones, there are protons, 54,55 Fe, 55 Co, and 56 Ni, while the main influencers are 54,55 Mn and 55−57 Fe, in disagreement with Parikh et al (2013), who found that SNIa nucleosynthesis is most sensitive to the β + -decay rates of 28 Si, 32 S, and 36 Ar. An eventual increase in all weak rates on pf-shell nuclei would affect the dynamical evolution of hot bubbles, running away at the beginning of the explosion, and the yields of SNIa.

show abstract

“…Future observations of Ti and Cr in 3C 397 will be interesting because the production of these elements in the n-NSE layer is very sensitive to the central density of the WD (e.g., Woosley 1997;Dave et al 2017;Leung & Nomoto 2018). 50 Ti and 52,54 Cr are produced at the deepest layers in near-M Ch explosions (see dashed green and solid purple curves in Figure 1).…”

Section: Nucleosynthesis For Other Type Ia Snrsmentioning

confidence: 99%

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

Sato

Bravo

Badenes

et al. 2020

ApJ

View full text Add to dashboard Cite

Chandra X-ray observations of Kepler's supernova remnant indicate the existence of a high speed Fe-rich ejecta structure in the southwestern region. We report strong K-shell emission from Fe-peak elements (Cr, Mn, Fe, Ni), as well as Ca, in this Fe-rich structure, implying that those elements could be produced in the inner area of the exploding white dwarf. We found Ca/Fe, Cr/Fe, Mn/Fe and Ni/Fe mass ratios of 1.0-4.1%, 1.0-4.6%, 1-11% and 2-30%, respectively. In order to constrain the burning regime that could produce this structure, we compared these observed mass ratios with those in 18 one-dimensional Type Ia nucleosynthesis models (including both near-M Ch and sub-M Ch explosion models). The observed mass ratios agree well with those around the middle layer of incomplete Si-burning in Type Ia nucleosynthesis models with a peak temperature of ∼(5.0-5.3)×10 9 K and a high metallicity, Z > 0.0225. Based on our results, we infer the necessity for some mechanism to produce protruding Fe-rich clumps dominated by incomplete Si-burning products during the explosion. We also discuss the future perspectives of X-ray observations of Fe-rich structures in other Type Ia supernova remnants.

show abstract

Constraining the Single-degenerate Channel of Type Ia Supernovae with Stable Iron-group Elements in SNR 3C 397

Cited by 33 publications

References 175 publications

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

Sensitivity of Type Ia supernovae to electron capture rates

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

Contact Info

Product

Resources

About

Constraining the Single-degenerate Channel of Type Ia Supernovae with Stable Iron-group Elements in SNR 3C 397

Cited by 33 publications

References 175 publications

The Intrinsic Stochasticity of the 56Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

The Intrinsic Stochasticity of the 56Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

Sensitivity of Type Ia supernovae to electron capture rates

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

Contact Info

Product

Resources

About

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia

The Intrinsic Stochasticity of the ⁵⁶Ni Distribution of Single-degenerate Near-Chandrasekhar-mass SN Ia