Status on $$^{\mathbf {12}}\mathbf {C}+{}^{\mathbf {12}}{\mathbf {C}}$$ fusion at deep subbarrier energies: impact of resonances on astrophysical $$S^{*}$$ factors

Beck, C.; Mukhamedzhanov, A. M.; Tang, Xiaodong

doi:10.1140/epja/s10050-020-00075-2

Cited by 40 publications

(33 citation statements)

References 42 publications

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“…Measurements of these have been performed at energies above E c.m. = 2.1 MeV, and three different extrapolation methods have been used to estimate the reaction cross section at lower energies (Beck, Mukhamedzhanov, & Tang 2020). Comparing to the standard rate CF88 from Caughlan & Fowler (1988), the indirect measurement using the Trojan Horse Method suggests an enhancement of the reaction rate due to a number of potential resonances in the unmeasured energy range (Tumino et al 2018), while the phenomenological 'hindrance model' suggests a greatly suppressed and lower rate (Jiang et al 2018).…”

Section: Uncertainties In the Relevant Reaction Ratesmentioning

confidence: 99%

The radioactive nuclei and in the Cosmos and in the solar system

Diehl

Lugaro

Heger

et al. 2021

Publ. Astron. Soc. Aust.

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The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently re-processes metal-enriched stellar ejecta into the next generation of stars. The study of cosmic nucleosynthesis and this matter cycle requires the understanding of the physics of nuclear reactions, of the conditions at which the nuclear reactions are activated inside the stars and stellar explosions, of the stellar ejection mechanisms through winds and explosions, and of the transport of the ejecta towards the next cycle, from hot plasma to cold, star-forming gas. Due to the long timescales of stellar evolution, and because of the infrequent occurrence of stellar explosions, observational studies are challenging, as they have biases in time and space as well as different sensitivities related to the various astronomical methods. Here, we describe in detail the astrophysical and nuclear-physical processes involved in creating two radioactive isotopes useful in such studies, $^{26}\mathrm{Al}$ and $^{60}\mathrm{Fe}$ . Due to their radioactive lifetime of the order of a million years, these isotopes are suitable to characterise simultaneously the processes of nuclear fusion reactions and of interstellar transport. We describe and discuss the nuclear reactions involved in the production and destruction of $^{26}\mathrm{Al}$ and $^{60}\mathrm{Fe}$ , the key characteristics of the stellar sites of their nucleosynthesis and their interstellar journey after ejection from the nucleosynthesis sites. This allows us to connect the theoretical astrophysical aspects to the variety of astronomical messengers presented here, from stardust and cosmic-ray composition measurements, through observation of $\gamma$ rays produced by radioactivity, to material deposited in deep-sea ocean crusts and to the inferred composition of the first solids that have formed in the Solar System. We show that considering measurements of the isotopic ratio of $^{26}\mathrm{Al}$ to $^{60}\mathrm{Fe}$ eliminate some of the unknowns when interpreting astronomical results, and discuss the lessons learned from these two isotopes on cosmic chemical evolution. This review paper has emerged from an ISSI-BJ Team project in 2017–2019, bringing together nuclear physicists, astronomers, and astrophysicists in this inter-disciplinary discussion.

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Section: Uncertainties In the Relevant Reaction Ratesmentioning

confidence: 99%

The radioactive nuclei and in the Cosmos and in the solar system

Diehl

Lugaro

Heger

et al. 2021

Publ. Astron. Soc. Aust.

Self Cite

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“…= 2.1 MeV with large uncertainties. Three different kinds of extrapolations have been used to estimate the reaction cross section at lower energies [192][193][194][195][196][197][198]. A recent 24 Mg(α, α ) 24 Mg experiment at RCNP provides important information for the resonances at stellar energies [199].…”

Section: Helium and Carbon Burningsmentioning

confidence: 99%

Progress in nuclear astrophysics of east and southeast Asia

Aziz

Ahmad²,

Ahn³

et al. 2021

AAPPS Bull.

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Nuclear astrophysics is an interdisciplinary research field of nuclear physics and astrophysics, seeking for the answer to a question, how to understand the evolution of the universe with the nuclear processes which we learn. We review the research activities of nuclear astrophysics in east and southeast Asia which includes astronomy, experimental and theoretical nuclear physics, and astrophysics. Several hot topics such as the Li problems, critical nuclear reactions and properties in stars, properties of dense matter, r-process nucleosynthesis, and ν-process nucleosynthesis are chosen and discussed in further details. Some future Asian facilities, together with physics perspectives, are introduced.

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“…In addition to this, there are resonant structures observed even at a very low energy region. As a result, large uncertainties persist in reaction rate while extrapolating the data at an astrophysically significant energy range (Beck et al (2020); Tan et al (2020)). So the experimental measurement of the fusion cross‐section for 12 C + 12 C fusion reaction has been limited to the energies above E c .…”

Section: Introductionmentioning

confidence: 99%

“…To extrapolate the data in the lower energy regions of astrophysical interest, the theoretical modeling of heavy‐ion 12 C + 12 C fusion reaction is necessary. Various phenomenological and microscopic models have been developed to explain the fusion dynamics of these heavy‐ion reactions (Beck et al (2020); Zhang et al (2020)). Further, to remove the effects arising due to the Coulomb barrier, the fusion cross‐section for astrophysical reactions is defined in terms of astrophysical S‐factor.…”

Section: Introductionmentioning

confidence: 99%

Fusion dynamics of ¹²C + ¹²C reaction: An astrophysical interest within the relativistic mean‐field approach

2021

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The 12 C + 12 C fusion reaction plays a significant role in the later phases of stellar evolution. For a better understanding of the evolution involved, one must understand the corresponding fusion-fission dynamics and reaction characteristics. In the present analysis, we have studied the fusion cross-section along with the S-factor for this reaction using the well-known M3Y and recently developed R3Y nucleon-nucleon (NN) potential along with the relativistic mean-field densities in double-folding approach. The density distributions and the microscopic R3Y NN potential are calculated using the NL3 * parameter set. Thesummed Wong model is employed to investigate the fusion cross-section, with max-values from the sharp cutoff model. The calculated results are also then compared with the experimental data. It is found that the R3Y interaction gives a reasonable agreement with the data.

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Status on $$^{\mathbf {12}}\mathbf {C}+{}^{\mathbf {12}}{\mathbf {C}}$$ fusion at deep subbarrier energies: impact of resonances on astrophysical $$S^{*}$$ factors

Cited by 40 publications

References 42 publications

The radioactive nuclei and in the Cosmos and in the solar system

The radioactive nuclei and in the Cosmos and in the solar system

Progress in nuclear astrophysics of east and southeast Asia

Fusion dynamics of ¹²C + ¹²C reaction: An astrophysical interest within the relativistic mean‐field approach

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Status on $$^{\mathbf {12}}\mathbf {C}+{}^{\mathbf {12}}{\mathbf {C}}$$ fusion at deep subbarrier energies: impact of resonances on astrophysical $$S^{*}$$ factors

Cited by 40 publications

References 42 publications

The radioactive nuclei and in the Cosmos and in the solar system

The radioactive nuclei and in the Cosmos and in the solar system

Progress in nuclear astrophysics of east and southeast Asia

Fusion dynamics of 12C + 12C reaction: An astrophysical interest within the relativistic mean‐field approach

Contact Info

Product

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Fusion dynamics of ¹²C + ¹²C reaction: An astrophysical interest within the relativistic mean‐field approach