Constraining the<sup>12</sup>C+<sup>12</sup>C fusion cross section for astrophysics

Bucher, B.; Fang, X.; Tang, Xiaodong; Tan, Wanpeng; Alongi, A.; Ayangeakaa, A. D.; Beard, M.; Best, A.; Browne, J.; Cahillane, C.; Couder, M.; Dahlstrom, E.; Davies, P.; deBoer, R. J.; Kontos, A.; Lamm, L. O.; Long, Alexander; Lu, Wenting; Lyons, S.; Ma, Chi; Moncion, Alexander; Notani, M.; Patel, D.; Paul, N.; Pignatari, M.; Roberts, A.; Robertson, Daniel; Smith, K.; Stech, E.; Talwar, R.; Thomas, Spencer A.; Wiescher, M.

doi:10.1051/epjconf/20159303009

Cited by 6 publications

(2 citation statements)

References 26 publications

(66 reference statements)

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“…Due to their importance for a variety of stellar environments, in particular in Type 1a SN studies, these reaction rates are currently under much investigation (e.g. Bucher et al 2015). Chen et al (2014) examined the impact of variations to the 12 C + 12 C rates on carbon burning within super-AGB stars and found that if the rates were multiplied by factors of 1 000 and 0.01, the minimum CO core mass for carbon ignition became 0.93 M and 1.10 M , respectively.…”

Section: Doherty Et Almentioning

confidence: 99%

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Doherty

Gil‐Pons

Siess

et al. 2017

Publ. Astron. Soc. Aust.

161

193

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We review the lives, deaths and nucleosynthetic signatures of intermediate-mass stars in the range ≈6-12 M , which form super-AGB stars near the end of their lives. The critical mass boundaries both between different types of massive white dwarfs (CO, CO-Ne, ONe), and between white dwarfs and supernovae, are examined along with the relative fraction of super-AGB stars that end life either as an ONe white dwarf or as a neutron star (or an ONeFe white dwarf), after undergoing an electron capture supernova event. The contribution of the other potential single-star channel to electroncapture supernovae, that of the failed massive stars, is also discussed. The factors that influence these different final fates and mass limits, such as composition, rotation, the efficiency of convection, the nuclear reaction rates, mass-loss rates, and third dredge-up efficiency, are described. We stress the importance of the binary evolution channels for producing electron-capture supernovae. Recent nucleosynthesis calculations and elemental yield results are discussed and a new set of s-process heavy element yields is presented. The contribution of super-AGB star nucleosynthesis is assessed within a Galactic perspective, and the (super-)AGB scenario is considered in the context of the multiple stellar populations seen in globular clusters. A brief summary of recent works on dust production is included. Last, we conclude with a discussion of the observational constraints and potential future advances for study into these stars on the low mass/high mass star boundary.

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Section: Doherty Et Almentioning

confidence: 99%

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Doherty

Gil‐Pons

Siess

et al. 2017

Publ. Astron. Soc. Aust.

161

193

View full text Add to dashboard Cite

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“…This resonance has been posited to explain the discrepancy between the observed and predicted superburst ignition depth, much in the way the Hoyle state was predicted to explain cosmic carbon production [207]. However, present experimental constraints are contradictory and rely on theoretical extrapolations [208].…”

Section: Nuclear Sensitivities and Recent Uncertainty Reduction Effortsmentioning

confidence: 99%

Nuclear physics of the outer layers of accreting neutron stars

Meisel

Deibel

Keek

et al. 2018

J. Phys. G: Nucl. Part. Phys.

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Now 50 years since the existence of the neutron star crust was proposed, we review the current understanding of the nuclear physics of the outer layers of accreting neutron stars. Nuclei produced during nuclear burning replace the nascent composition of the neutron star ocean and crust. Non-equilibrium nuclear reactions driven by compression alter the outer thermal structure and chemical composition, leaving observable imprints on astronomical phenomena. As observations of bursting neutron stars and cooling neutron stars have increased, the recent volume of astronomical data allows new insights into the microphysics of the neutron star interior and the possibility to test nuclear physics input in model calculations. Despite numerous advances in our understanding of neutron star interiors and observed neutron star phenomena, many challenges remain in the astrophysics theory of accreting neutron stars, the nuclear theory of neutron-rich nuclei, and the reach and precision of terrestrial nuclear physics experiments. Nuclear Physics of the Outer Layers of Accreting Neutron StarsFor example, current investigations of the critical reaction rates in X-ray bursts [9,27], studies of key properties of nuclei in the accreted crust [25,26], and nuclear reaction network calculations of accreted crust compositions [22,24,28], all promise to improve the observational constraints on dense matter derived from accreting neutron stars.We begin in section 2 by briefly outlining the neutron star structure. Sections 3 and 4 describe the original composition of the neutron star crust and the accretion process which drives the system from equilibrium. In section 5, we discuss the nuclear burning that can occur on the surface of accreting neutron stars and the nuclei produced during the different possible burning regimes. In actively accreting neutron stars, the ashes of prior surface nuclear burning are compressed to greater depths by newly accreted material. We discuss in section 6 the nuclear interactions involving the ashes that take place as the ambient mass density increases. In section 7, we investigate the impact of interior nuclear interactions on observable neutron star phenomena. We summarize and discuss prospects for future work in section 8.

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Direct measurements of the ¹²C(¹²C,p)²³Na and ¹²C(¹²C,α)²⁰Ne reactions at low energies for Nuclear Astrophysics

et al. 2022

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12C+12C reactions are crucial in the evolution of massive stars and explosive scenarios. The measurement of these reactions at astrophysical energies is very challenging due to their extremely small cross sections, and the presence of beam induced background originated by the natural 1,2H contaminants in the C targets. In addition, the many discrepancies between different data sets and the complicated resonant structure of the cross sections make the extrapolation to low energies very uncertain. Recently, we performed a direct measurement of the 12C+12C reactions at the CIRCE Laboratory in Italy. Results from a study on target contamination were used, allowing us to measure cross sections at Ec.m. =2.51 − 4.36 MeV with 10-25 keV energy steps. Two stage ΔE-Erest detectors were used for unambiguous particle identiﬁcation. Branching ratios of individual particle groups were found to vary signiﬁcantly with energy and angular distributions were also found to be anisotropic, which could be a potential explanation for the discrepancies observed among different data sets.

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Constraining the¹²C+¹²C fusion cross section for astrophysics

Cited by 6 publications

References 26 publications

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Nuclear physics of the outer layers of accreting neutron stars

Direct measurements of the ¹²C(¹²C,p)²³Na and ¹²C(¹²C,α)²⁰Ne reactions at low energies for Nuclear Astrophysics

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Constraining the12C+12C fusion cross section for astrophysics

Cited by 6 publications

References 26 publications

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Nuclear physics of the outer layers of accreting neutron stars

Direct measurements of the 12C(12C,p)23Na and 12C(12C,α)20Ne reactions at low energies for Nuclear Astrophysics

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Constraining the¹²C+¹²C fusion cross section for astrophysics

Direct measurements of the ¹²C(¹²C,p)²³Na and ¹²C(¹²C,α)²⁰Ne reactions at low energies for Nuclear Astrophysics