An Expanding Shell of Neutral Hydrogen Associated with SN 1006: Hints for the Single-Degenerate Origin and Faint Hadronic Gamma-Rays

Sano, H.; Yamaguchi, H.; Aruga, M.; Fukui, Y.; Tachihara, K.; Filipovic, M. D.; Rowell, G.

doi:10.48550/arxiv.2205.13712

Cited by 2 publications

(2 citation statements)

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“…If we adopt n p = 230 cm −3 and d = 1.4 kpc, we find W p ∼5.3 × 10 47 erg, which corresponds to ∼0.05% of the total kinetic energy released by a SNe. Figure 9 shows a plot between the SNR age and W p (Sano et al 2021a(Sano et al ,b, 2022, and indicates that Puppis A is located in a position consistent with the cosmic-ray escaping phase suggested by the other more than ten SNRs (Sano et al 2022). We consider a significant part of the CR protons have escaped from the SNR shell in the time scale 10 4 yr.…”

Section: Estimation Of the Cosmic Ray Energy From The Hadronic Gamma-...mentioning

confidence: 85%

Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A

Aruga¹,

Sano²,

Fukui³

et al. 2022

Preprint

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We have carried out a study of the interstellar medium (ISM) toward a shell-like supernova remnant SNR Puppis A by using the NANTEN CO and ATCA Hi data. We synthesized a comprehensive picture of the SNR radiation by combining the ISM data with the gamma-ray and X-ray distributions. The ISM, both atomic and molecular gas, is dense and highly clumpy, and is distributed along the northeastern edge of the SNR shell. The CO distribution revealed an enhanced line intensity ratio of CO(J = 2-1)/(J = 1-0) transitions as well as CO line broadening, which indicate shock heating/acceleration. The results support that Puppis A is located at 1.4 kpc. The ISM interacting with the SNR has large mass of ∼10 4 M which is dominated by Hi, showing good spatial correspondence with the Fermi-LAT gamma-ray image. This favors the hadronic origin of the gamma-rays, while additional contribution of the leptonic component is not excluded. The distribution of the X-ray ionization timescales within the shell suggests that the shock front ionized various parts of the ISM at epochs ranging over a few to ten 1000 yr. We therefore suggest that the age of the SNR is around 10 4 yr as given by the largest ionization timescale. We estimate the total cosmic ray energy W p to be 10 47 erg, which is well placed in the cosmic-ray escaping phase of an age-W p plot including more than ten SNRs.

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Section: Estimation Of the Cosmic Ray Energy From The Hadronic Gamma-...mentioning

confidence: 85%

Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A

Aruga¹,

Sano²,

Fukui³

et al. 2022

Preprint

Self Cite

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“…The community is far from a consensus on the leading SN Ia scenario(s). Therefore, studies continue to explore each one of these stellar binary scenarios (e.g., some examples from the last two years, Cui et al 2020;Zou et al 2020;Ablimit 2021;Blondin et al 2021;Chandra et al 2021;Clark et al 2021;Liu et al 2021;Meng & Luo 2021;Michaely 2021;Wang et al 2021;Yamaguchi et al 2021;Zeng et al 2021;Ablimit 2022;Acharova et al 2022;Chu et al 2022;Cui & Li 2022;Dimitriadis et al 2022;Ferrand et al 2022;Lach et al 2022;Liu et al 2022;Livneh & Katz 2022;Mazzali et al 2022;Pakmor et al 2022;Patra et al 2022;Piersanti et al 2022;Rau & Pan 2022;Ruiz-Lapuente et al 2022;Sano et al 2022;Sharon & Kushnir 2022;Shingles et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Pre-explosion Helium Shell Flash in Type Ia Supernovae

Soker¹

2022

Res. Astron. Astrophys.

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I study the possibility that within the frame of the core degenerate (CD) scenario for type Ia supernovae (SNe Ia) the merger process of the core of the asymptotic giant branch (AGB) star and the white dwarf (WD) maintains an envelope mass of $\approx 0.03 M_\odot$ that causes a later helium shell flash. I estimate the number of pre-explosion helium shell flash events to be less than few per cents of all CD scenario SNe Ia. A helium shell flash while the star moves to the left on the HR diagram as a post-AGB star (late thermal pulse---LTP) or along the WD cooling track (very-LTP) causes the star to expand and become a `born again’ AGB star. Merger remnants exploding while still on the AGB form \add{hydrogen-polluted} peculiar SNe Ia, while an explosion inside an inflated born-again star results in an early flux excess in the light curve of the SN Ia. The fraction of systems that might show an early flux excess due to LTP/VLTP is $< {\rm few} \times 10^{-4}$ of all SNe Ia, much below the observed fraction. In the frame of the CD scenario SNe Ia with early flux excess result from SN ejecta collision with planetary nebula fallback gas, or from mixing of $^{56}$Ni to the outer regions of the SN ejecta. Ongoing sky surveys might find about one case per year where LTP/VLTP influences the SN light curve.

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An Expanding Shell of Neutral Hydrogen Associated with SN 1006: Hints for the Single-Degenerate Origin and Faint Hadronic Gamma-Rays

Cited by 2 publications

References 87 publications

Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A

Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A

Pre-explosion Helium Shell Flash in Type Ia Supernovae

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