Abstract :
[en] Context. Thanks to the vast and exquisite set of observations that have been made available for the Sun, our star is by far an ideal
target for testing stellar models with a unique precision. A recent issue under consideration in the field is related to the progress in
the solar surface abundances derivation that has led to a decrease of the solar metallicity. While the former high-metallicity models
were in fair agreement with other observational indicators from helioseismology and solar neutrino fluxes, it is no longer the case
for low-metallicity models. This issue has become known as ’the solar problem’. Recent data are, however, promising to shed a new
light on it. For instance, in 2020, the Borexino collaboration released the first-ever complete estimate of neutrinos emitted in the
CNO cycle, which has reaffirmed the role of the neutrino constraints in the solar modelling process and their potential in exploring
related issues. In parallel, a newly claimed detection of solar gravity modes of oscillation offers another opportunity for probing the
stratification in the Sun’s central layers.
Aims. We propose combining the diagnoses from neutrinos and helioseismology, both from pressure and gravity modes, in assessing
the predictions of solar models. We compare in detail the different physical prescriptions currently at our disposal with regard to stellar
model computations.
Methods. We built a series of solar standard models based on a variation of the different physical ingredients directly affecting the
core structure: opacity, chemical mixture, nuclear reactions rates. We compare the predictions of these models to their observational
counterparts for the neutrinos fluxes, gravity-mode period spacing, and low-degree pressure mode frequency ratios.
Results. The CNO neutrino flux confirms previous findings, exhibiting a preference for high-metallicity models. Nevertheless, we
found that mild modification of the nuclear screening factors can re-match low-metallicity model predictions to observed fluxes, al-
though it does not restore the agreement with the helioseismic frequency ratios. Neither the high-metallicity or low-metallicity models
are able to reproduce the gravity-mode period spacing. The disagreement is huge, more than 100σ to the observed value. Reversely,
the family of standard models narrows the expected range of the Sun’s period spacing: between ∼2150 to ∼2190 s. Moreover, we
show this indicator can constrain the chemical mixture, opacity, and – to a lower extent – nuclear reactions in solar models.
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