Determination of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Be</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>9</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>(α,<i>n</i><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>)</mml:mo></mml:mrow><mml:mrow><mml:mn>12</mml:mn></mml:mrow></mml:m

Kunz, R.; Barth, S.; Denker, A.; Drotleff, H. W.; Hammer, J. W.; Knee, H.; Mayer, A.

doi:10.1103/physrevc.53.2486

Cited by 26 publications

(21 citation statements)

References 11 publications

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“…The atmosphere is a grey Eddington model. Nuclear reactions rates were taken from the (updated) JINA REACLIB (Cyburt et al 2010) -with the exception of the 9 Be(α,n) 12 C reaction, which is taken from Kunz et al (1996) -under weak (Salpeter) screening (Salpeter 1954), which provides a more fitting description of the solar process (Gruzinov & Bahcall 1998) than the other already implemented methods.…”

Section: Input Physicsmentioning

confidence: 99%

“…Since then, solar neutrino experiments themselves have more recently began to emerge as a potential probe of regions traditionally inaccessible to helioseismology (Lopes & Turck-Chièze 2013). Neutrinos are also hypothesized to be relevant to the determination of the density of the solar core (Lopes 2013), something that will be especially relevant when measurements sensitive enough to detect matter oscillations start to be obtained for more sources, and something helioseismic techniques are sensitive to.…”

Section: Introductionmentioning

confidence: 99%

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The impact of composition choices on solar evolution: age, helio- and asteroseismology, and neutrinos

Capelo

Lopes

2020

Monthly Notices of the Royal Astronomical Society

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The Sun is the most studied and well-known star, and as such, solar fundamental parameters are often used to bridge gaps in the knowledge of other stars, when these are required for modelling. However, the two most powerful and precise independent methodologies currently available to infer the internal solar structure are in disagreement. We aim to show the potential impact of composition choices in the overall evolution of a star, using the Sun as example. To this effect, we create two Standard Solar Models and a comparison model using different combinations of metallicity and relative element abundances and compare evolutionary, helioseismic, and neutrino-related properties for each. We report differences in age for models calibrated to the same point on the HR-diagram, in red giant branch, of more than 1 Gyr, and found that the current precision level of asteroseismic measurements is enough to differentiate these models, which would exhibit differences in period spacing of 1.30% to 2.58%. Additionally, we show that the measurement of neutrino fluxes from the CNO cycle with a precision of around 17%, which could be achieved by the next generation of solar neutrino experiments, could help resolve the stellar abundance problem.

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Section: Input Physicsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The impact of composition choices on solar evolution: age, helio- and asteroseismology, and neutrinos

Capelo

Lopes

2020

Monthly Notices of the Royal Astronomical Society

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“…leaving the 12 C in its ground state) and n 1 (when the 12 C residual nucleus is populated in its E x = 4.44 MeV state) channels extracted from Refs. [27][28][29]. The n 1 data was normalized by a factor of 0.52 as discussed in Ref.…”

Section: Construction Of Data Setsmentioning

confidence: 99%

Analysis of excited states in ¹³C and their cluster structure

Lombardo

2019

EPJ Web Conf.

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An accurate understanding of the spectroscopy of 13C is key to understand clustering phenomena in light nuclear systems. In this nucleus, many theoretical models predict the existence of α-cluster configurations, stabilized by the presence of an extra neutron. Despite of its importance, the spectroscopy of13C is still affected by ambiguities, demanding for new data against which benchmarking the models. We improve the knowledge on the 13C level scheme by means of a comprehensive R-matrix analysis of several experimental data sets. Our new spectroscopic information contributes to solve existing ambiguities in 13C structure and will serve a valid benchmark for theoretical models attempting to describe clustering in neutron rich systems.

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“…The simple and non-destructive method for evidencing Be-treatment proposed here relies on the well-known 9 Be(a, nc) 12 C nuclear reaction using a helium ion beam impinging on the gem placed in air and recording the 4439 keV prompt c-ray tagging Be atoms [4]. The cross section of the reaction 9 Be(a, nc) 12 C monotonically increases from 0.5 MeV [5] to 1.7 MeV [6,7], where it reaches a maximum (fraction of barn). This reaction has been formerly used to monitor traces of beryllium in the environment with a source of alpha particles of 5 MeV emitted by a 210 Po source of 0.16 Ci [8].…”

Section: Introductionmentioning

confidence: 99%