Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere

By E. Caffau, H. Ludwig, M. Steffen, Bernd Freytag, P. Bonifacio. 2010

626 citations recorded by the source corpus.

In the last decade, the photospheric solar metallicity as determined from spectroscopy experienced a remarkable downward revision. Part of this effect can be attributed to an improvement of atomic data and the inclusion of NLTE computations, but also the use of hydrodynamical model atmospheres seemed to play a role. This “decrease” with time of the metallicity of the solar photosphere increased the disagreement with the results from helioseismology. With a CO5BOLD 3D model of the solar atmosphere, the CIFIST team at the Paris Observatory re-determined the photospheric solar abundances of several elements, among them C, N, and O. The spectroscopic abundances are obtained by fitting the equivalent width and/or the profile of observed spectral lines with synthetic spectra computed from the 3D model atmosphere. We conclude that the effects of granular fluctuations depend on the characteristics of the individual lines, but are found to be relevant only in a few particular cases. 3D effects are not responsible for the systematic lowering of the solar abundances in recent years. The solar metallicity resulting from this analysis is Z=0.0153, Z/X=0.0209.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/588056128605c742991c3256aade8cf298d53f5a

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In Astronomy and Astrophysics

1. C. Conroy
2. R. Dav'e
3. Michela Mapelli
4. R. Somerville
5. P. Hopkins
6. S. Charlot
7. Eric Mamajek
8. L. Hernquist

In Atmospheric Science

1. Martin Asplund
2. N. Grevesse
3. M. Bergemann
4. J. Laming
5. D. Reames
6. K. Lind
7. A. Sauval
8. Pat Scott

Citations in the corpus

• New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, background): “According to Caffau et al. (2011), the presentday Sun’s metallicity is Z = 0.01524, intermediate between the most recent estimates, e.g.”
• HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, neutral): “32 The Astrophysical Journal, 804:64 (38pp), 2015 May 1 Mann et al. Asplund et al. 2009; Caffau et al. 2011).”
• A non-LTE study of neutral and singly-ionized iron line spectra in 1D models of the Sun and selected late-type stars ? (2011, methodology): “Our 1D Fe ii based abundance (the non-LTE effects are negligible) is 0.04 dex lower compared with log εFeII = 7.512 ± 0.062 obtained by Caffau et al. (2011) from their solar 3D analysis when using g f -values from Meléndez & Barbuy (2009) in both studies.”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “0.015 (e.g., Asplund et al. 2009; Lodders et al. 2009; Caffau et al. 2011).”
• Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths (2015, methodology): “We adopt the same relative abundances of heavy elements as in G15, taken from Bressan et al. (2012, largely based on Caffau et al. 2011) for solar metallicity.”
• A spectroscopic survey of Herbig Ae/Be stars with X-shooter – I. Stellar parameters and accretion rates (2015, methodology): “The PARSEC tracks of Bressan et al. (2012) are used for the majority of this step as they cover a mass range of 0.1– 12M⊙, which encompasses all of the theoretical HAeBe mass range, and a metallicity is chosen of Z=0.01 (this is close to solar metallicity (Caffau et al. 2011)).”
• The elemental composition of the Sun - III. The heavy elements Cu to Th (2014, methodology): “Caffau et al. (2011a) recently redetermined the solar abundance of Zr using their 3D model.”
• A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, methodology): “We adopt Z⊙ ≡ MZ,⊙/M⊙ = 0.0153 from Caffau et al. (2011) and show the range of Z⊙ = 0.013 to 0.0168 from Bahcall et al. (2005) as possible sources of uncertainty.”
• The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “A reanalysis of Asplund et al. (2009) results and the use of an independent set of solar model atmospheres (see, e.g., Caffau et al. 2011, for a detailed discussion) has provided a solar heavy element distribution intermediate between those by Grevesse & Sauval (1998) and Asplund et al. (2009).”
• The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “…1 we collect the recommended solar photospheric abundances of various commonly observed elements from Grevesse and Sauval (1998), Asplund et al. (2009), (also given in Grevesse et al., 2010) Caffau et al. (2011), and Scott et al. (2014b,a) and Grevesse et al. (2014) for comparison and reference.”
• Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code (2017, methodology): “In SEVN and throughout this paper, we use Z = 0.01524 for solar metallicity (Caffau et al. 2011).”
• Star formation in semi-analytic galaxy formation models with multiphase gas (2015, methodology): “We have converted the observed values of 12+ log(O/H) to Z/Z⊙ assuming 12 + log(O/H) = 8.76 for the Sun (Caffau et al. 2011), and Zg/Z⊙ = (O/H)/(O/H)⊙.”
• Spectroscopic analysis of DA white dwarfs with 3D model atmospheres (2013, methodology): “These models are part of the CIFIST grid (Ludwig et al. 2009; Caffau et al. 2011; Tremblay et al. 2013b) along with giant and dwarf simulations computed by the Paris GEPI group.”
• A NEW GENERATION OF PARSEC-COLIBRI STELLAR ISOCHRONES INCLUDING THE TP-AGB PHASE (2017, background): “The reference solar-scaled composition is taken from Caffau et al. (2011).”