Constraining Solar Abundances Using Helioseismology

By S. Basu, H. M. Antia. 2004

194 citations recorded by the source corpus.

Recent analyses of solar photospheric abundances suggest that the oxygen abundance in the solar atmosphere needs to be revised downward. In this study, we investigate the consequence of this revision on helioseismic analyses of the depth of the solar convection zone and the helium abundance in the solar envelope and find no significant effect. We also find that the revised abundances along with the current OPAL opacity tables are not consistent with seismic data. A significant upward revision of the opacity tables is required to make solar models with lower oxygen abundance consistent with seismic observations.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/a24c2386ad2fefb557bb83c5b313de37f9e47263

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Citations in the corpus

The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, background): “These values have to be compared with the asteroseismic estimates RCZ/R⊙ = 0.713± 0.001 (Basu 1997) and Y⊙,surf = 0.2485± 0.0035 (Basu & Antia 2004).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “The helium surface abundance at 4.57 Gyr in the best solar model is much lower compared to the helioseismologically inferred value of 0.2485±0.0034 (Basu & Antia 2004).”
Helioseismology and Solar Abundances (2007, methodology): “Of course the result were based on models that had the then accepted value of Z/X, i.e., 0.0245.”
The Adequacy of Stellar Evolution Models for the Interpretation of the Color-Magnitude Diagrams of Resolved Stellar Populations (2005, background): “Assuming these, Basu & Antia (2004) derive Y 0.2486.”
Helioseismological Implications of Recent Solar Abundance Determinations (2004, methodology): “Basu & Antia (2004) discussed the characteristics of a solar envelope model which invoked, in order to satisfy helioseismic constraints, a 19% increase in radiative opacity relative to the tabulated OPAL opacities.”
Solar Neutrinos: Status and Prospects (2012, background): “…to observation: the radius of the convective zone boundary RCZ , the interior sound speed and density profiles, and the surface He abundance YS all move outside the ranges determined from helioseismic analyses (Bahcall, Serenelli & Pinsonneault 2004; Basu & Antia 2004; Montalban et al. 2004).”
NEW SOLAR COMPOSITION: THE PROBLEM WITH SOLAR MODELS REVISITED (2009, background): “…be- tween models and helioseismic inferences has prompted a number of authors to revise the physical inputs of SSMs (Montalbán et al. 2004; Basu & Antia 2004; Bahcall et al. 2005; Guzik 2006; Christensen-Dalsgaard et al. 2009), and to question the revision of the solar abundances,…”
The Solar Chemical Composition (2004, methodology): “The present-day photospheric abundance of helium adopted is obtained from inversion of helioseismic data by Basu and Antia (2004): Y , the abundance by mass of He, is Y = 0.2485.”
SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, background): “The entries in the table should be compared to the helioseismic values, RCZ = 0.713 ± 0.001 (Basu & Antia 1997) and 0.2485±0.0035 (Basu & Antia 2004), respectively.”
New Solar Opacities, Abundances, Helioseismology, and Neutrino Fluxes (2004, background): “A number of authors have pointed out that these lower heavy element abundances lead to solar models that conflict with different aspects of helioseismological measurements (e.g., Bahcall & Pinsonneault 2004, Basu & Antia 2004, Bahcall et al. 2005).”
The chemical composition of the Sun (2009, methodology): “3.9): YS ≈ 0.238 compared with the observed 0.2485 ± 0.0034 (Basu & Antia 2004), where YS is the present-day He mass fraction at the surface.”
A New Generation of Standard Solar Models (2016, background): “This solar abundance problem (Basu & Antia 2004; Bahcall et al. 2005b; Delahaye & Pinsonneault 2006) has defied a complete solution.”
CESAM: a free code for stellar evolution calculations (2008, background): “Model E is based on the AGS05 solar mixture which makes the agreement between the solar model and helioseismic observations much worse (see for instance Basu & Antia, 2004).”
A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers (2007, background): “We note that these abundances are currently a topic of debate (e.g., Basu & Antia 2004; Bahcall et al. 2005a,b), and the solar C and O abundances could be ≈ 0.2 dex higher.”
Updated opacities from the Opacity Project (2004, background): “papers to be necessary to increase opacities in the vicinity of RCZ: by 19% according to Basu and Antia (2004); and by 21% according to Bahcall et al. (2004a).”
10,000 Standard Solar Models: A Monte Carlo Simulation (2005, background): “For comparison with the value given in Table 6, the helioseismologically determined depth of the convective zone is (Kosovichev & Fedorova 1991; Christensen-Dalsgaard et al. 1991; Guzik & Cox 1993; Basu & Antia 1997, 2004; Basu 1998): RCZ = 0.713± 0.001R⊙ .”