A CHANDRASEKHAR MASS PROGENITOR FOR THE TYPE Ia SUPERNOVA REMNANT 3C 397 FROM THE ENHANCED ABUNDANCES OF NICKEL AND MANGANESE

Yamaguchi, Hiroya; Badenes, Carles; Foster, Adam; Bravo, Eduardo; Williams, Brian J.; Maeda, Keiichi; Nobukawa, Masayoshi; Eriksen, Kristoffer A.; Brickhouse, N. S.; Petre, Robert; Koyama, K.

doi:10.1088/2041-8205/801/2/l31

Cited by 131 publications

(198 citation statements)

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“…The SD model is thought to have observable consequences and some classes of SD models have been observationally ruled out as the dominant channel (e.g., Leonard 2007;Bianco et al 2011;Chomiuk et al 2016;Maguire et al 2016), but there are a number of systems that are considered to be candidate progenitor systems (e.g. U Sco and V445 Pup; Li et al 2011) and there might be multiple channels for producing normal SNe Ia (e.g., Maguire et al 2013;Yamaguchi et al 2015). Current explosion simulations of both SD (e.g.…”

Section: Introductionmentioning

confidence: 99%

Whimper of a Bang: Documenting the Final Days of the Nearby Type Ia Supernova 2011fe

Shappee

Stanek

Kochanek

et al. 2017

ApJ

123

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Using the Hubble Space Telescope (HST) and the Large Binocular Telescope, we followed the evolution of the Type Ia supernova (SN Ia) 2011fe for an unprecedented 1840 days past B-band maximum light and over a factor of 7 million in flux. At 1840 days, the 4000 -17000 Å quasi-bolometric luminosity is just (420 ± 20) L . By measuring the late-time quasi-bolometric light curve, we present the first confident detection of 57 Co decay in a SN Ia light curve and estimate a mass ratio of log( 57 Co/ 56 Co) = −1.59 +0.06 −0.07 . We do not have a clean detection of 55 Fe, but find a limit of 55 Fe/ 57 Co < 0.22 with 99% confidence. These abundance ratios provide unique constraints on the progenitor system because the central density of the exploding white dwarf(s) dictates these nucleosynthetic yields. The observed ratios strongly prefer the lower central densities of doubledegenerate models ( 55 Fe/ 57 Co = 0.27) over the higher central densities of near-Chandrasekhar-mass singledegenerate models ( 55 Fe/ 57 Co = 0.68). However, additional theoretical studies predicting isotopic yields from a broader range of progenitor systems are motivated by these unique observations. We will continue to observe SN 2011fe for another ∼ 600 days with HST and possibly beyond.

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Section: Introductionmentioning

confidence: 99%

Whimper of a Bang: Documenting the Final Days of the Nearby Type Ia Supernova 2011fe

Shappee

Stanek

Kochanek

et al. 2017

ApJ

123

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“…For models with the same ρ c , increasing Z leads to a growth in both ratios; for models with the same Z, increasing ρ c shows similar results but at a steeper rate. We include the data from the remnant 3C 397 [20], which is known to have a high [Mn/Fe] ratio. In [20], one-dimensional SNIa models are explored to explain such feature.…”

Section: Resultsmentioning

confidence: 99%

“…We include the data from the remnant 3C 397 [20], which is known to have a high [Mn/Fe] ratio. In [20], one-dimensional SNIa models are explored to explain such feature. It is found that metallicity > 5Z ⊙ is required to explain such feature.…”

Section: Resultsmentioning

confidence: 99%

“…We use the Helmholtz equation of states, which contains contributions from ideal electron gas of arbitrarily relativistic and degenerate levels, blackbody photon gas, ions with Coulomb interactions and positron-electron annihilation pairs [4]. To describe the nuclear reactions, we use a 7-isotope network coupled with the simulations, including 4 He, 12 C, 16 O, 20 Ne, 24 Mg, 28 Si and 56 Ni [5]. We use the turbulent deflagration model [6] with delayed detonation transition [7].…”

Section: Methodsmentioning

confidence: 99%

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Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Leung¹,

Nomoto²

2017

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

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The observed features of typical Type Ia supernovae are well-modeled as the explosions of carbonoxygen white dwarfs both near Chandrasekhar mass and sub-Chandrasekhar mass. However, observations in the last decade have shown that Type Ia supernovae exhibit a wide diversity, which implies models for wider range of parameters are necessary. Based on the hydrodynamics code we developed, we carry out a parameter study of Chandrasekhar mass models for Type Ia supernovae. We conduct a series of two-dimensional hydrodynamics simulations of the explosion phase using the turbulent flame model with the deflagration-detonation-transition (DDT). To reconstruct the nucleosynthesis history, we use the particle tracer scheme. We examine the role of model parameters by examining their influences on the final product of nucleosynthesis. The parameters include the initial density, metallicity, initial flame structure, detonation criteria and so on. We show that the observed chemical evolution of galaxies can help constrain these model parameters. KEYWORDS:Type Ia supernovae, hydrodynamics, nucleosynthesis MethodWe carry out two-dimensional hydrodynamics simulations [1] by solving the Euler equations in cylindrical coordinates. The spatial and temporal discretization are calculated by the fifth-order weighted essentially non-oscillatory (WENO) scheme [2] and the five-step third-order non-strong stability preserving Runge-Kutta scheme [3]. We use the Helmholtz equation of states, which contains contributions from ideal electron gas of arbitrarily relativistic and degenerate levels, blackbody photon gas, ions with Coulomb interactions and positron-electron annihilation pairs [4]. To describe the nuclear reactions, we use a 7-isotope network coupled with the simulations, including 4 He, 12 C, 16 O, 20 Ne, 24 Mg, 28 Si and 56 Ni [5]. We use the turbulent deflagration model [6] with delayed detonation transition [7]. The flame and detonation are described by the level-set scheme [8]. The laminar flame and detonation speed are taken from [9] and calculated using the scheme in [10]. The energy production by the explosion follows the three-step scheme as in [11], which includes carbon burning, nuclear quasi-statistical equilibrium (NQSE) burning and NSE burning. In NSE burning, electron capture is included.To calculate the detailed nucleosynthesis, we use the torch nuclear reaction subroutine which consists of 495 isotopes from 1 H to 91 Tc [12]. The nuclear reaction rates are taken from [13] and [14]. Weak interaction rates of iron-peaked elements are obtained from [15], whereas other isotopes are obtained from [16]. We perform a parameter survey to study the influences of model parameters based on a benchmark model, which satisfies three criteria: 1. Healthy 56 Ni production about 0.6 solar mass; 2. Consistency of the 55 Mn to the galactic chemical evolution; 3. Agreement of 58 Ni with the solar abundance.

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“…In the evolved Galactic SNR 3C 397, Yamaguchi et al (2015) found high ratios of Ni/Fe and Mn/Fe in the X-ray spectrum. As seen in Figure 2, the Ni/Fe and Mn/Fe ratios are among the highest reported for Type Ia SNRs, and strongly indicate that the progenitor must have exploded close to M Ch , which is more naturally explained by the SD scenario.…”

Section: Type Ia Snr -Progenitor Connectionsmentioning

confidence: 93%

Supernova Remnants as Clues to Their Progenitors

Patnaude¹,

Badenes²

2017

Handbook of Supernovae

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Supernovae shape the interstellar medium, chemically enrich their host galaxies, and generate powerful interstellar shocks that drive future generations of star formation. The shock produced by a supernova event acts as a type of time machine, probing the mass loss history of the progenitor system back to ages of ∼ 10 000 years before the explosion, whereas supernova remnants probe a much earlier stage of stellar evolution, interacting with material expelled during the progenitor's much earlier evolution. In this chapter we will review how observations of supernova remnants allow us to infer fundamental properties of the progenitor system. We will provide detailed examples of how bulk characteristics of a remnant, such as its chemical composition and dynamics, allow us to infer properties of the progenitor evolution. In the latter half of this chapter, we will show how this exercise may be extended from individual objects to SNR as classes of objects, and how there are clear bifurcations in the dynamics and spectral characteristics of core collapse and thermonuclear supernova remnants. We will finish the chapter by touching on recent advances in the modeling of massive stars, and the implications for observable properties of supernovae and their remnants.

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A CHANDRASEKHAR MASS PROGENITOR FOR THE TYPE Ia SUPERNOVA REMNANT 3C 397 FROM THE ENHANCED ABUNDANCES OF NICKEL AND MANGANESE

Cited by 131 publications

References 50 publications

Whimper of a Bang: Documenting the Final Days of the Nearby Type Ia Supernova 2011fe

Whimper of a Bang: Documenting the Final Days of the Nearby Type Ia Supernova 2011fe

Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Supernova Remnants as Clues to Their Progenitors

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