Exploration of Aspherical Ejecta Properties in Type Ia Supernovae: Progenitor Dependence and Applications to Progenitor Classification

Leung, Shing-Chi; Diehl, R.; Nomoto, Ken’ichi; Siegert, Thomas

doi:10.3847/1538-4357/abc9c1

Cited by 7 publications

(3 citation statements)

References 158 publications

(229 reference statements)

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“…SN 2014J is the only SN Ia in the last few decades which has been detected in γ-ray. Early gamma-ray signals around 10 days detected after explosion and the observed line velocity of 56 Co (Diehl et al 2015) has provided indication on the explosion asymmetry (Leung et al 2021b) (but also see Churazov et al (2015) for other interpretations).…”

Section: Observations and Motivationmentioning

confidence: 93%

A New Versatile Code for Gamma-Ray Monte-Carlo Radiative Transfer

Leung¹

2022

Preprint

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The developments in modeling of instrumental background for MeV telescopes such as INTEGRAL/SPI and Fermi/GBM, as well as new gamma-ray projects such as the accepted COSI and the proposed e-ASTROGAM and AMEGO missions, suggest the potential of observing elusive transients. This allows testing the stellar explosion mechanisms and their corresponding nucleosynthesis through short-lived radioactive isotopes with improved sensitivity and accuracy. This raises for the need of a radiative transfer code which may efficiently explore different types of astrophysical γ-ray sources and their dependence on model parameters and input physics. In view of this, we present our new Monte-Carlo Radiative Transfer code in Python. The code synthesizes the spectra and light curves suitable for modeling supernova ejecta. We test the code extensively for reproducing results consistent with analytic models, in particular for scenarios including C+O novae, O+Ne novae, Type Ia and core-collapse supernovae. We also compare our results with similar models in the literature and discuss how our code depends on selected input physics and setting.

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Section: Observations and Motivationmentioning

confidence: 93%

A New Versatile Code for Gamma-Ray Monte-Carlo Radiative Transfer

Leung¹

2022

Preprint

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“…The successful detonation is mainly limited to the heaviest core mass of M CO = 1.1 M e . In the context of a onedimensional problem, it is thus indicated that direct ignition of detonation on a helium envelope with 0.02 M e (to avoid conflicts to observational properties; Shen et al 2021;Woosley & Kasen 2011) is extremely difficult for the progenitors of M CO = 0.9-1.0 M e , which are favorable for normal SNe type Ia (Shigeyama et al 1992;Sim et al 2010;Woosley & Kasen 2011;Leung et al 2021).…”

Section: Progenitor Conditions For Ignitionmentioning

confidence: 99%

One-dimensional Numerical Study on Ignition of the Helium Envelope in Dynamical Accretion during the Double-degenerate Merger

Iwata

Maeda

2022

ApJ

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In order for a double-detonation model to be viable for normal type Ia supernovae, the adverse impact of helium-burning ash on early time observables has to be avoided, which requires that the helium envelope mass should be at most 0.02 M ⊙. Most of the previous studies introduced detonation by artificial hot spots, and therefore the robustness of the spontaneous helium detonation remains uncertain. In the present work, we conduct a self-consistent hydrodynamic study on the spontaneous ignition of the helium envelope in the context of the double-degenerate channel, by applying an idealized one-dimensional model and a simplified seven-isotope reaction network. We explore a wide range of the progenitor conditions and demonstrate that the chance of direct initiation of detonation is limited. Especially, the spontaneous detonation requires the primary envelope mass of ≳0.03 M ⊙. Ignition as deflagration is instead far more likely, which is feasible for the lower envelope mass down to ∼0.01 M ⊙, which might lead to subsequent detonation once the deflagration-to-detonation transition (DDT) is realized. High-resolution multidimensional simulations are required to further investigate the DDT possibility, as well as accurately derive the threshold between the spontaneous detonation and deflagration ignition regimes. Another interesting finding is the effect of the composition: while mixing with the core material enhances detonation as previously suggested, it rather narrows the chance for deflagration due to the slower rate of the 12C(α,γ)16O reaction at the lower temperature ∼108K, with the caveat that we presently neglect the proton-catalyzed reaction sequence of 12C(p,γ)13O(α,p)16O.

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“…The shocked dense gas can also greatly enhance the X-ray flux. Although it does not necessarily rule out the factor of intrinsic explosion asymmetry (see, e.g., Ferrand et al 2019;Leung et al 2021, for application of using explosion asymmetry in constraining explosion mechanism), at least the ISM environment plays a significant role in the formation of the asymmetric morphology of SNR G306.3−0.9.…”

Section: Origin Of Asymmetrymentioning

confidence: 99%

Spatially Resolved X-Ray Study of Supernova Remnant G306.3–0.9 with Unusually High Calcium Abundance

Weng

Zhou

Chen

et al. 2022

ApJ

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G306.3–0.9 is an asymmetric Galactic supernova remnant (SNR), whose progenitor has been thought to be a Type Ia supernova (SN), but its high Ca abundance appears inconsistent with the Type Ia origin. Hoping to uncover the reason for its asymmetry and the origin of this SNR, we performed a spatially resolved X-ray spectroscopic analysis of XMM-Newton and Chandra observation data. We divided the SNR into 13 regions and analyzed the spectra using two-temperature models (0.2 keV + 1 keV). Compared to the southwestern regions, the northeastern regions have higher metal abundances and a lower gas density. This suggests that the asymmetric morphology results from the nonuniform ambient environment. We found that neither Type Ia nor core-collapse SN models can account for the abnormally high abundance ratios of Ar/Si, Ca/Si, or the shape of the abundance curve. A comparison with the Ca-rich transient models suggests that G306.3–0.9 is likely to be the first identified Galactic Ca-rich transient remnant, although the theoretical production of element S is lower. We also note that the conclusion for the SNR’s origin relies on the measured abundance ratios and existing nucleosynthesis models. Between two groups of Ca-rich transient explosion models, we prefer the He shell detonation for an accreting white dwarf, rather than the merger of a white dwarf and a neutron star.

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Exploration of Aspherical Ejecta Properties in Type Ia Supernovae: Progenitor Dependence and Applications to Progenitor Classification

Cited by 7 publications

References 158 publications

A New Versatile Code for Gamma-Ray Monte-Carlo Radiative Transfer

A New Versatile Code for Gamma-Ray Monte-Carlo Radiative Transfer

One-dimensional Numerical Study on Ignition of the Helium Envelope in Dynamical Accretion during the Double-degenerate Merger

Spatially Resolved X-Ray Study of Supernova Remnant G306.3–0.9 with Unusually High Calcium Abundance

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