The solar interior

Gough, D. O.; Scherrer, P. H.

doi:10.1007/978-94-010-0320-9_44

Cited by 6 publications

(2 citation statements)

References 117 publications

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“…Additional properties of the model can be constrained by further equations of stellar structure combined with suitably chosen aspects of the physics of the stellar interior (Antia and Chitre 1997;Takata and Shibahashi 1998). Such a model, based on using Model S as reference, was presented by Gough and Scherrer (2001), with the underlying analysis and further details discussed by Gough (2004). The analysis constrained the composition and temperature structure based on the nuclear energy-generation rate.…”

Section: Investigations Of the Structure And Physics Of The Solar Interiormentioning

confidence: 99%

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: Investigations Of the Structure And Physics Of The Solar Interiormentioning

confidence: 99%

Solar structure and evolution

Christensen‐Dalsgaard

2021

Living Rev Sol Phys

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“…To do so, a promising approach is to try to rebuild the solar structure as seen from helioseismic data, as done in e.g. Shibahashi et al (1995), Shibahashi & Takata (1996), Basu & Thompson (1996) , Gough & Scherrer (2001), Gough (2004) and Turck-Chièze et al (2004), and use this static structure to provide insights on potential revision of key ingredients of solar and stellar models. In this paper, we present a new approach to rebuild the solar structure based on inversions of the Ledoux discriminant, defined as…”

Section: Introductionmentioning

confidence: 99%

Seismic Solar Models from Ledoux discriminant inversions

Buldgen,

Eggenberger,

Baturin

et al. 2020

Preprint

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Context. The Sun constitutes an excellent laboratory of fundamental physics. With the advent of helioseismology, we were able to probe its internal layers with unprecendented precision and thoroughness. However, the current state of solar modelling is still stained by tedious issues. One of these central problems is related to the disagreement between models computed with recent photospheric abundances and helioseismic constraints. The observed discrepancies raise questions on some fundamental ingredients entering the computation of solar and stellar evolution models. Aims. We use solar evolutionary models as initial conditions for reintegrations of their structure using Ledoux discriminant inversions. The resulting models are defined as seismic solar models, satisfying the equations of hydrostatic equilibrium. These seismic models will allow us to better constrain the internal structure of the Sun and provide complementary information to that of calibrated standard and non-standard models. Methods. We use inversions of the Ledoux discriminant to reintegrate seismic solar models satisfying the equations of hydrostatic equilibrium. These seismic models were computed using various reference models with different equations of state, abundances and opacity tables. We check the robustness of our approach by confirming the good agreement of our seismic models in terms of sound speed, density and entropy proxy inversions as well as frequency-separation ratios of low-degree pressure modes. Results. Our method allows us to determine with an excellent accuracy the Ledoux discriminant profile of the Sun and compute full profiles of this quantity. Our seismic models show an agreement with seismic data of ≈ 0.1% in sound speed, density and entropy proxy after 7 iterations in addition to an excellent agreement with the observed frequency-separation ratios. They surpass all standard and non-standard evolutionary models including ad-hoc modifications of their physical ingredients aiming at reproducing helioseismic constraints. Conclusions. The obtained seismic Ledoux discriminant profile as well as the full consistent structure obtained from our reconstruction procedure paves the way for renewed attempts at constraining the solar modelling problem and the missing physical processes acting in the solar interior by breaking free from the hypotheses of evolutionary models.

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Isotopic Composition of H, He and Ne in the Protosolar Cloud

Geiss

Gloeckler

2003

Solar System History From Isotopic Signatures of Volatile Elements

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The solar interior

Cited by 6 publications

References 117 publications

Solar structure and evolution

Solar structure and evolution

Seismic Solar Models from Ledoux discriminant inversions

Isotopic Composition of H, He and Ne in the Protosolar Cloud

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