Using the standard solar model to constrain solar composition and nuclear reaction<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>S</mml:mi></mml:math>factors

We perform a quantitative analysis of the solar composition problem by using a statistical approach that allows us to combine the information provided by helioseimic and solar neutrino data in an effective way. We include in our analysis the helioseismic determinations of the surface helium abundance and of the depth of the convective envelope, the measurements of the 7 Be and 8 B neutrino fluxes, the sound speed profile inferred from helioseismic frequencies. We provide all the ingredients to describe how these quantities depend on the solar surface composition and to evaluate the (correlated) uncertainties in solar model predictions. We include errors sources that are not traditionally considered such as those from inversion of helioseismic data. We, then, apply the proposed approach to infer the chemical composition of the Sun. We show that the opacity profile of the Sun is well constrained by the solar observational properties. In the context of a two parameter analysis in which elements are grouped as volatiles (i.e. C, N, O and Ne) and refractories (i.e Mg, Si, S, Fe), the optimal composition is found by increasing the the abundance of volatiles by (45 ± 4) % and that of refractories by (19 ± 3) % with respect to the values provided by Asplund et al. (2009). This corresponds to the abundances ε O = 8.85 ± 0.01 and ε Fe = 7.52 ± 0.01. As an additional result of our analysis, we show that the observational data prefer values for the input parameters of the standard solar models (radiative opacities, gravitational settling rate, the astrophysical factors S 34 and S 17 ) that differ at the ∼ 1σ level from those presently adopted.

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“…with the δI values summarized in Serenelli et al (2013). The only exception is the opacity, that we discuss below.…”

Section: Theoretical Uncertaintiesmentioning

confidence: 99%

“…B Q,I values are available at Serenelli et al (2013) for all observables except the sound speed c(r).…”

Section: Theoretical Uncertaintiesmentioning

confidence: 99%

The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

Villante¹,

Serenelli²,

Delahaye³

et al. 2014

ApJ

145

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“…In the most updated SSM calculation, the present precision of the 14 N(p, γ) 15 O crosssection is 7.2% (i.e. S 1,14 (0) = 1.66 ± 0.12 keV b) and, as a consequence, the uncertainties due to the S 1,14 and S 1,7 (7.7%) are dominating the SSM uncertainties for the nuclear rates [76]. Presently, a solar abundance problem is present: if the recently measured low metallicity values [77] are used as inputs in the SSM instead of the values reported in [78], then SSM predictions are no more in agreement with helioseismology data.…”

Section: Thementioning

confidence: 99%

The nuclear physics of the hydrogen burning in the Sun

2016

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Abstract. Underground nuclear astrophysics focuses its efforts towards a deeper knowledge of the nuclear reactions that rule stellar evolution processes and enable the synthesis of the elements of the periodic table. Deep underground in the Gran Sasso laboratory, the cross-sections of the key reactions of the hydrogen burning have been measured right down to the energies of astrophysical interest. The main results obtained by the LUNA Collaboration are reviewed, and their contributions to the solution of the solar neutrino problem and to the age of the globular cluster are discussed.

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“…3.3), particle physicist are now scrutinizing the data for deviations from this standard three-flavor scenario, searching for instance for signs of non-standard neutrino interactions [14,15] or mixing of active with ultra-light sterile neutrinos [16]. On the other hand, solar physics will profit from more precise flux data on all spectral components [17], especially regarding the neutrinos from the subdominant CNO fusion cycle for which currently only upper limits exist [18].…”

Section: Introductionmentioning

confidence: 99%

Solar neutrino spectroscopy

Wurm

2017

Physics Reports

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More than forty years after the first detection of neutrinos from the Sun, the spectroscopy of solar neutrinos has proven to be an on-going success story. The long-standing puzzle about the observed solar neutrino deficit has been resolved by the discovery of neutrino flavor oscillations. Today's experiments have been able to solidify the standard MSW-LMA oscillation scenario by performing precise measurements over the whole energy range of the solar neutrino spectrum.This article reviews the enabling experimental technologies: On the one hand mutlikiloton-scale water Cherenkov detectors performing measurements in the high-energy regime of the spectrum, on the other end ultrapure liquid-scintillator detectors that allow for a lowthreshold analysis. The current experimental results on the fluxes, spectra and time variation of the different components of the solar neutrino spectrum will be presented, setting them in the context of both neutrino oscillation physics and the hydrogen fusion processes embedded in the Standard Solar Model.Finally, the physics potential of state-of-the-art detectors and a next-generation of experiments based on novel techniques will be assessed in the context of the most interesting open questions in solar neutrino physics: a precise measurement of the vacuum-matter transition curve of electron-neutrino oscillation probability that offers a definitive test of the basic MSW-LMA scenario or the appearance of new physics; and a first detection of neutrinos from the CNO cycle that will provide new information on solar metallicity and stellar physics.

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Using the standard solar model to constrain solar composition and nuclear reactionSfactors

Cited by 59 publications

References 27 publications

The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

The nuclear physics of the hydrogen burning in the Sun

Solar neutrino spectroscopy

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