Combining multiple structural inversions to constrain the solar modelling problem

Buldgen, G.; Salmon, Sébastien; Noels, A.; Scuflaire, R.; Montalbán, J.; Батурин, В. А.; Eggenberger, P.; Gryaznov, V. K.; Iosilevskiy, Igor; Meynet, Georges; Chaplin, W. J.; Miglio, A.; Oreshina, A. V.; Richard, Olivier; Starostin, A. N.

doi:10.1051/0004-6361/201833971

Cited by 28 publications

(44 citation statements)

References 115 publications

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“…Table 4) from the value 7.93 quoted by AGSS09 to 8.08. As shown by Buldgen et al (2019b) the resulting increase in the opacity (see also Fig. 5) results in a modest increase in the depth of the convection zone and the envelope helium abundance, although still far from enough to match the observed values.…”

Section: Possible Corrections To the Solar Modelsmentioning

confidence: 55%

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Solar structure and evolution

Christensen‐Dalsgaard

2021

Living Rev Sol Phys

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The Sun provides a critical benchmark for the general study of stellar structure and evolution. Also, knowledge about the internal properties of the Sun is important for the understanding of solar atmospheric phenomena, including the solar magnetic cycle. Here I provide a brief overview of the theory of stellar structure and evolution, including the physical processes and parameters that are involved. This is followed by a discussion of solar evolution, extending from the birth to the latest stages. As a background for the interpretation of observations related to the solar interior I provide a rather extensive analysis of the sensitivity of solar models to the assumptions underlying their calculation. I then discuss the detailed information about the solar interior that has become available through helioseismic investigations and the detection of solar neutrinos, with further constraints provided by the observed abundances of the lightest elements. Revisions in the determination of the solar surface abundances have led to increased discrepancies, discussed in some detail, between the observational inferences and solar models. I finally briefly address the relation of the Sun to other similar stars and the prospects for asteroseismic investigations of stellar structure and evolution.

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Section: Possible Corrections To the Solar Modelsmentioning

confidence: 55%

“…A comprehensive analysis of solar modelling and helioseismic diagnostics was carried out by Buldgen et al (2019b). The modelling used the GN93, GS98 and AGSS09 compositions, a range of different opacity tables, and different equations of state.…”

Section: Possible Corrections To the Solar Modelsmentioning

confidence: 99%

Solar structure and evolution

Christensen‐Dalsgaard

2021

Living Rev Sol Phys

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“…Thus, the change in the photospheric metallicity of the Sun is significant enough to impact the discussion of the solar modelling problem (Castro et al 2007;Guzik & Mussack 2010;Serenelli et al 2011;Buldgen et al 2019). The estimate given by Asplund et al (2009), that is, Z = 0.0134, cannot be explained by our models.…”

Section: The Peculiar Composition Of the Sunmentioning

confidence: 83%

The solar abundance problem and eMSTOs in clusters

Hoppe

Bergemann

Bitsch

et al. 2020

A&A

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In this study, we focus on the impact of accretion from protoplanetary discs on the stellar evolution of AFG-type stars. We used a simplified disc model that was computed using the Two-Pop-Py code, which contains the growth and drift of dust particles in the protoplanetary disc, to model the accretion scenarios for a range of physical conditions for protoplanetary discs. Two limiting cases were combined with the evolution of stellar convective envelopes that were computed using the Garstec stellar evolution code. We find that the accretion of metal-poor (gas) or metal-rich (dust) material has a significant impact on the chemical composition of the stellar convective envelope. As a consequence, the evolutionary track of the star diverts from the standard scenario predicted by canonical stellar evolution models, which assume a constant and homogeneous chemical composition after the assembly of the star is complete. In the case of the Sun, we find a modest impact on the solar chemical composition. Indeed, the accretion of metal-poor material reduces the overall metallicity of the solar atmosphere and it is consistent, within the uncertainty, with the solar Z reported by Caffau et al. (2011, Sol. Phys., 268, 255), but our model is not consistent with the measurement by Asplund et al. (2009, ARA&A, 47, 481). Another relevant effect is the change of the position of the star in the colour-magnitude diagram. By comparing our predictions with a set of open clusters from the Gaia DR2, we show that it is possible to produce a scatter close to the TO of young clusters that could contribute to explaining the observed scatter in CMDs. Detailed measurements of metallicities and abundances in the nearby open clusters will additionally provide a stringent observational test for our proposed scenario.

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“…These approaches can be used to robustly infer global properties (e.g. mean density, see [37,182]), but also to build specific proxies [34][35][36]186] of stellar structure designed to test key ingredients of stellar physics related to, e.g., microscopic diffusion, convective boundary mixing (see Section 2.1). -The signature of activity cycles can be found in frequency shifts / modes' lifetimes changes as a function of time (e.g., [85,117,189,195]).…”

Section: Preamble -What Can We Infer From High-precision High-cadencmentioning

confidence: 99%

Haydn

Miglio

Girardi

Grundahl³

et al. 2021

Exp Astron

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In the last decade, the Kepler and CoRoT space-photometry missions have demonstrated the potential of asteroseismology as a novel, versatile and powerful tool to perform exquisite tests of stellar physics, and to enable precise and accurate characterisations of stellar properties, with impact on both exoplanetary and Galactic astrophysics. Based on our improved understanding of the strengths and limitations of such a tool, we argue for a new small/medium space mission dedicated to gathering high-precision, high-cadence, long photometric series in dense stellar fields. Such a mission will lead to breakthroughs in stellar astrophysics, especially in the metal poor regime, will elucidate the evolution and formation of open and globular clusters, and aid our understanding of the assembly history and chemodynamics of the Milky Way’s bulge and a few nearby dwarf galaxies.

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Combining multiple structural inversions to constrain the solar modelling problem

Cited by 28 publications

References 115 publications

Solar structure and evolution

Solar structure and evolution

The solar abundance problem and eMSTOs in clusters

Haydn

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