The Seismic Structure of the Sun

Gough, D. O.; Kosovichev, A. G.; Toomre, J.; Anderson, E.; Antia, H. M.; Basu, Sarbani; Chaboyer, Brian; Chitre, S. M.; Christensen‐Dalsgaard, J.; Dziembowski, W. A.; Eff-Darwich, A.; Elliott, J. Richard; Giles, P. M.; Goode, Philip R.; Guzik, Joyce A.; Harvey, J. W.; Hill, F.; Leibacher, J. W.; Monteiro, M. J. P. F. G.; Richard, Olivier; Sekii, T.; Shibahashi, Hiromoto; Takata, Masasuke; Thompson, M. J.; Vauclair, S.; Vorontsov, S. V.

doi:10.1126/science.272.5266.1296

Cited by 226 publications

(137 citation statements)

References 27 publications

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“…In this the case of rotation differs from the case of solar structure, where the theoretical models have been found to agree reasonably well with the inferred sound speed and density (e.g., Gough et al 1996;Basu et al 1997;Turck-Chieze et al 2001). This is perhaps not surprising.…”

Section: Solar Rotation From Helioseismologymentioning

confidence: 83%

The Internal Solar Rotation from Helioseismology

Christensen‐Dalsgaard

2004

Symp. - Int. Astron. Union

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Helioseismology has provided detailed inferences about the internal rotation of the Sun, and hence stringent constraints on any attempt to understand the properties and evolution of stellar rotation. Here I briefly discuss the techniques used in the analysis and review the results that have been obtained. Strikingly, these results are markedly different from the predictions made before the helioseismic data became available, emphasizing the difficulties in the modelling of phenomena as complex as stellar internal rotation.

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Section: Solar Rotation From Helioseismologymentioning

confidence: 83%

The Internal Solar Rotation from Helioseismology

Christensen‐Dalsgaard

2004

Symp. - Int. Astron. Union

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“…This result has been obtained by many authors, in di erent ways (see Gough et al (1996) and references therein). There is a characteristic discrepancy of order one percent, just below the convective zone, between the sound velocity computed in the models and that of the seismic Sun.…”

Section: Evidence Of Element Settling Inside the Sun From Helioseismomentioning

confidence: 86%

“…Discussion : necessity of mild mixing, 7 Li and 3 He Although the introduction of pure element settling in the solar models considerably improves the consistency with the \seismic Sun", some discrepancies do remain, particularly below the convective zone where a "spike" appears in the sound velocity (see Gough et al 1996). The helium pro les directly obtained from helioseismology (Basu 1997, Antia andChitre 1997) Dotted line: without element settling; solid line: with settling computed for helium and 14 other elements (from Richard, Vauclair and Charbonnel, 1998) show indeed a helium gradient below the convection zone which is smoother than the gradient obtained with pure settling.…”

Section: Evidence Of Element Settling Inside the Sun From Helioseismomentioning

confidence: 99%

Element Settling in the Solar Interior

Vauclair¹

1998

Solar Composition and Its Evolution — From Core to Corona

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Abstract.Element settling inside the Sun now becomes detectable from the comparison of the observed oscillation modes with the results of the theoretical models. This settling is due, not only to gravitation, but also to thermal di usion and radiative acceleration (although this last e ect is small compared to the two others ). It leads to abundance variations of helium and heavy elements of = 10% below the convective zone. Although not observable from spectroscopy, such v ariations lead to non-negligible modi cations of the solar internal structure and evolution. Helioseismology is a powerful tool to detect such e ects, and its positive results represent a great success for the theory of stellar evolution. Meanwhile, evidences are obtained that the element settling is slightly smoothed down, probably due to mild macroscopic motions below the convective zone. Additional observations of the abundances of both 7 Li and 3 He lead to speci c constraints on these particular motions.

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“…The inferences about the solar internal structure obviously provide a strong test of modelling of stellar evolution. Although earlier solar models were in reasonable, but far from perfect, agreement with the helioseismic determinations (Gough et al 1996), recent redeterminations of the solar surface abundance have led to a very substantial increase in the discrepancies between the Sun and the model (for reviews, see Guzik 2006Guzik , 2008Basu & Antia 2008, see also Section 4.1).…”

Section: Introductionmentioning

confidence: 99%

Prospects for asteroseismology

Christensen‐Dalsgaard¹,

Houdek²

2009

Synergies Between Solar and Stellar Modelling

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The observational basis for asteroseismology is being dramatically strengthened, through more than two years of data from the CoRoT satellite, the flood of data coming from the Kepler mission and, in the slightly longer term, from dedicated ground-based facilities. Our ability to utilize these data depends on further development of techniques for basic data analysis, as well as on an improved understanding of the relation between the observed frequencies and the underlying properties of the stars. Also, stellar modelling must be further developed, to match the increasing diagnostic potential of the data. Here we discuss some aspects of data interpretation and modelling, focussing on the important case of stars with solar-like oscillations.

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The Seismic Structure of the Sun

Cited by 226 publications

References 27 publications

The Internal Solar Rotation from Helioseismology

The Internal Solar Rotation from Helioseismology

Element Settling in the Solar Interior

Prospects for asteroseismology

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