Constraining Solar Abundances Using Helioseismology

Basu, Sarbani; Antia, H. M.

doi:10.1086/421110

Cited by 270 publications

(393 citation statements)

References 19 publications

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“…Its abundance can be inferred from the solar wind and corona, but the value is poorly-constrained and highly variable. Theoretical models of stellar evolution and the data from helioseismology (Basu and Antia, 2004) provide a more accurate estimate, consistent with each other to 10% (see below); • light elements Li, B, and B are determined from the solar spectrum. The important lines, are, however, model dependent: because of very low abundances and very simple electronic configurations, the atoms give rise to one or few spectral lines only (Li I) or they are located in a very problematic part of a spectrum (Be II, B I).…”

Section: Methodsmentioning

confidence: 66%

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Solar Abundance Problem

Bergemann

Serenelli

2014

Determination of Atmospheric Parameters of B-, a-, F- And G-Type Stars

103

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The chemical composition of the Sun is among the most important quantities in astrophysics. Solar abundances are needed for modelling stellar atmospheres, stellar structure and evolution, population synthesis, and galaxies as a whole. The solar abundance problem refers to the conflict of observed data from helioseismology and the predictions made by stellar interior models for the Sun, if these models use the newest solar chemical composition obtained with 3D and NLTE models of radiative transfer. Here we take a close look at the problem from observational and theoretical perspective. We also provide a list of possible solutions, which have yet to be tested.

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Section: Methodsmentioning

confidence: 66%

“…Theoretical methods include inversions of helioseismic data (e.g. Basu and Antia, 2004) and nucleosynthesis models for heavy noble gases (e.g. Asplund et al, 2009).…”

Section: Methodsmentioning

confidence: 99%

Solar Abundance Problem

Bergemann

Serenelli

2014

Determination of Atmospheric Parameters of B-, a-, F- And G-Type Stars

103

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“…The He mass fraction Y is smaller than that in previous compilations, but the (rounded) He abundance is the same for the three compilations in Table 4. The hydrogen mass fraction of X=0.739 (Basu & Anita 2004) adopted here is essentially the same as in A05/G07, and the smaller value for GS98 seems to be due to the different model assumptions for deriving the He abundance there. Overall, the mass fractions derived here are closer to the ~10 year old GS98 compilation than to the most recent ones by L03, A05 or G07.…”

Section: Mass Fractions X Y and Z In Present-day Solar Materialsmentioning

confidence: 98%

“…Basu & Anita (2004, 2008 have shown that the estimated mass faction of H from helioseismic models is relatively independent on Z/X ratios in the range of 0.0171 < Z/X < 0.0245. Their models calibrated to Z/X=0.0171 and 0.0218 yield an average X=0.7389±0.0034 (Basu & Anita 2004). If the H mass fraction is indeed independent of the Z/X ratio, and if compositional variations within Z (mainly governed by the mass fractions of O, C, Ne, see below) also do not alter this conclusion much, we can use this X to estimate the He mass fraction.…”

Section: Mass Fractions X Y and Z In Present-day Solar Materialsmentioning

confidence: 99%

Solar System Abundances of the Elements

Lodders

2010

Astrophysics and Space Science Proceedings

275

176

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Summary. Representative abundances of the chemical elements for use as a solar abundance standard in astronomical and planetary studies are summarized. Updated abundance tables for solar system abundances based on meteorites and photospheric measurements are presented.Keywords: solar system abundances, solar photosphere, meteorites, CI chondrites Motivations to Study Solar System Elemental AbundancesThe investigations of what chemical elements exist in nature and in which quantities have a long history. The determination of elemental abundances in various celestial objects is still a very active field in astronomy, planetary science, and meteoritics. There are multiple motivations for studying the solar system abundances of the chemical elements. One reason to study this overall composition of the solar system is to understand how the diversity of planetary compositions, including that of our home planet, can be explained, since all planets in the solar system share a common origin from the material of the protosolar disk (the solar nebula).The composition of the sun determines how the sun works and evolves over time, as composition influences the interior structure of the sun. Although the Sun is mainly composed of H and He, other heavy elements such as C, N, O, Ne, Fe, etc., are important opacity sources that influence the energy transport out of the sun through radiation and convection. The sun is a typical main sequence dwarf star and its composition is a useful baseline for comparison to abundances in other dwarf stars and to changes that appear in advanced stages of stellar evolution. For example, relative to the sun's composition, red giant stars show observable abundance variations that are the result of nucleosynthesis operating in giant stars, and these products have been dredged up from stellar interiors to the stellar exteriors. 3The solar system abundances are a useful local galactic abundance standard because many nearby dwarf stars are similar in composition; however, in detail there are some stochastic abundance variations (e.g., Edvardsson et al. 1993, Nordstrom et al. 2004, Reddy et al. 2003, 2006. The term "cosmic" abundances should be avoided because abundances generally decrease with galactocentric distance. There are also abundance differences between our galaxy and galaxies at high red-shift; hence there is no generic "cosmic" composition that applies to all cosmic systems.Finally, solar abundances are a critical test of nucleosynthesis models and models of Galactic chemical evolution. Ideally, such models should quantitatively explain the elemental and nuclide distributions of solar system matter.The sun has the most mass (>99%) of the solar system objects and therefore it is the prime target for studying solar system abundances. Most elements can be measured in the sun's photosphere, but data from the solar chromosphere and corona, solar energetic particles, solar wind, and solar cosmic rays (from solar flares), help to evaluate abundances of elements that have weak absorption lines (bec...

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“…9) of the glitch, and with an amplitude which depends on the amplitude of the glitch and which decays with ν once the inverse radial wavenumber of the mode becomes comparable with or less than the radial extent of the glitch. Various approximate formulae for the oscillatory components that are associated with the helium ionization have been suggested and used, by e.g., Basu et al (1994); Basu & Antia (2004), Monteiro & Thompson (1998, 2005, and Gough (2002), not all of which are derived directly from explicit acoustic glitches. Gough used an analytic function for modelling the dip in the first adiabatic exponent γ 1 = (∂ ln p/∂ ln ρ) s , where p, ρ and s are pressure, density and specific entropy.…”

Section: Diagnostics Of Acoustic Glitchesmentioning

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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Constraining Solar Abundances Using Helioseismology

Cited by 270 publications

References 19 publications

Solar Abundance Problem

Solar Abundance Problem

Solar System Abundances of the Elements

Prospects for asteroseismology

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