Impact of New Gamow–teller Strengths on Explosive Type Ia Supernova Nucleosynthesis

Mori, Kanji; Famiano, M.; Kajino, Toshitaka; Suzuki, Toshio; Hidaka, Jun; Honma, Michio; Iwamoto, K.; Nomoto, Ken’ichi; Otsuka, Takaharu

doi:10.3847/1538-4357/833/2/179

Cited by 36 publications

(55 citation statements)

References 74 publications

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“…Studies of nucleosynthesis of one-dimensional models have shown some important dependencies on the model parameters. For example, Fe-peak elements synthesized in the Chandrasekhar mass model W7 (Nomoto et al 1984) is shown to be consistent with the solar abundances, except for a significant overproduction of 58 Ni, where the rate of electron capture is important (e.g., Thielemann et al 1986;Iwamoto et al 1999;Brachwitz et al 2000;Mori et al 2016). The solar abundance pattern of Fe-peak elements can also be reproduced by the sub-Chandra models with solar metallcity (e.g., Shigeyama et al 1992;Nomoto et al 1994), although the Ni/Fe ratio (which depends on metallicity) tends to be under solar because of the low central den-sity of exploding WDs.…”

Section: Introductionmentioning

confidence: 93%

“…Due to the availability of new electron capture rates, where the rates for iron-peak elements are in general lower, it is interesting to see if the overproduction problems in the W7 and WDD2 can be alleviated. This is also a study of how the abundance ratios among iron-peak elements depend on electron capture rates and possibly other nuclear reaction rates in view of still existing uncertainties of these rates (see also Mori et al 2016).…”

Section: Effects Of Updated Electron Capture Rates In 1-d Models Wmentioning

confidence: 99%

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Explosive Nucleosynthesis in Near-Chandrasekhar-mass White Dwarf Models for Type Ia Supernovae: Dependence on Model Parameters

Leung

Nomoto

2018

ApJ

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130

141

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We present two-dimensional hydrodynamics simulations of near-Chandrasekhar mass white dwarf (WD) models for Type Ia supernovae (SNe Ia) using the turbulent deflagration model with deflagrationdetonation transition (DDT). We perform a parameter survey for 41 models to study the effects of the initial central density (i.e., WD mass), metallicity, flame shape, DDT criteria, and turbulent flame formula for a much wider parameter space than earlier studies. The final isotopic abundances of 11 C to 91 Tc in these simulations are obtained by post-process nucleosynthesis calculations. The survey includes SNe Ia models with the central density from 5 × 10 8 g cm −3 to 5 × 10 9 g cm −3 (WD masses of 1.30 -1.38 M ⊙ ), metallicity from 0 to 5 Z ⊙ , C/O mass ratio from 0.3 -1.0 and ignition kernels including centered and off-centered ignition kernels. We present the yield tables of stable isotopes from 12 C to 70 Zn as well as the major radioactive isotopes for 33 models. Observational abundances of 55 Mn, 56 Fe, 57 Fe and 58 Ni obtained from the solar composition, well-observed SNe Ia and SN Ia remnants are used to constrain the explosion models and the supernova progenitor. The connection between the pure turbulent deflagration model and the subluminous SNe Iax is discussed. We find that dependencies of the nucleosynthesis yields on the metallicity and the central density (WD mass) are large. To fit these observational abundances and also for the application of galactic chemical evolution modeling, these dependencies on the metallicity and WD mass should be taken into account.

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Section: Introductionmentioning

confidence: 93%

Section: Effects Of Updated Electron Capture Rates In 1-d Models Wmentioning

confidence: 99%

Explosive Nucleosynthesis in Near-Chandrasekhar-mass White Dwarf Models for Type Ia Supernovae: Dependence on Model Parameters

Leung

Nomoto

2018

ApJ

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130

141

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“…On the other hand, Parikh et al (2013) analysed one threedimensional model of SNIa and the classical one-dimensional W7 model (Thielemann et al 1986), and found maximal sensitivity of SNIa nucleosynthesis to the electron capture rates of the α elements 28 Si, 32 S, and 36 Ar, whereas electron captures on IGN had little impact on the explosion. Recently, Mori et al (2016) have studied the impact that recent alternatives to the shell model calculations of Dean et al (1998), motivated by new experimental data on the electron capture rates on 56 Ni and 55 Co, have on SNIa nucleosynthesis. These data call for differences in the GT + strength distribution, leading to reduced electron capture rates.…”

Section: Introductionmentioning

confidence: 99%

“…These data call for differences in the GT + strength distribution, leading to reduced electron capture rates. Mori et al (2016) found that the overall yields of the explosion are affected at most by 2−3%. Both Mori et al (2016) and Parikh et al (2013) based their sensitivity study on modifying the nuclear rates in nuclear post-processing, meaning that the sensitivity study was decoupled from the supernova hydrodynamics.…”

Section: Introductionmentioning

confidence: 99%

Sensitivity of Type Ia supernovae to electron capture rates

Bravo

2019

A&A

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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.

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“…In this case, the over-production factor is suppressed within twice for all neutron-excess Cr, Fe and Ni isotopes [14]. Thus, the over-production problem of neutron-excess iron-group nuclei compared with the solar abundances is coming near to be solved.…”

Section: Nucleosynthesis Of Iron-group Nuclei In Type-ia Supernova Exmentioning

confidence: 98%

Electron-capture Rates for pf-shell Nuclei in Stellar Environments and Nucleosynthesis

Suzuki¹,

Honma²,

Mori³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Gamow-Teller strengths in p f -shell nuclei obtained by a new shell-model Hamltonian, GXPF1J, are used to evaluate electron-capture rates in p f -shell nuclei at stellar environments. The nuclear weak rates with GXPF1J, which are generally smaller than previous evaluations for proton-rich nuclei, are applied to nucleosynthesis in type Ia supernova explosions. The updated rates are found to lead to less production of neutron-rich nuclei such as 58 Ni and 54 Cr, thus toward a solution of the problem of over-production of neutron-rich isotopes of iron-group nuclei compared to the solar abundance.

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Impact of New Gamow–teller Strengths on Explosive Type Ia Supernova Nucleosynthesis

Cited by 36 publications

References 74 publications

Explosive Nucleosynthesis in Near-Chandrasekhar-mass White Dwarf Models for Type Ia Supernovae: Dependence on Model Parameters

Explosive Nucleosynthesis in Near-Chandrasekhar-mass White Dwarf Models for Type Ia Supernovae: Dependence on Model Parameters

Sensitivity of Type Ia supernovae to electron capture rates

Electron-capture Rates for pf-shell Nuclei in Stellar Environments and Nucleosynthesis

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