The photospheric solar oxygen project. III. Investigation of the centre-to-limb variation of the 630 nm [O I]-Ni I blend

  title={The photospheric solar oxygen project. III. Investigation of the centre-to-limb variation of the 630 nm [O I]-Ni I blend},
  author={Elisabetta Caffau and Hans-G. Ludwig and M. Steffen and William Charles Livingston and Piercarlo Bonifacio and Jean-Marie Malherbe and H. P. Doerr and W. Schmidt},
  journal={Astronomy and Astrophysics},
Context. The solar photospheric abundance of oxygen is still a matter of debate. For about ten years some determinations have favoured a low oxygen abundance which is at variance with the value inferred by helioseismology. Among the oxygen abundance indicators, the forbidden line at 630 nm has often been considered the most reliable even though it is blended with a Ni i line. In Papers I and II of this series we reported a discrepancy in the oxygen abundance derived from the 630 nm and the… 
The photospheric solar oxygen project: IV. 3D-NLTE investigation of the 777 nm triplet lines
The solar photospheric oxygen abundance is still widely debated. Adopting the solar chemical composition based on the "low" oxygen abundance, as determined with the use of three-dimensional (3D)
Uncertainties in the solar photospheric oxygen abundance
The purpose of this work is to better understand the confidence limits of the photospheric solar oxygen abundance derived from three-dimensional models using the forbidden [OI] line at 6300 \AA ,
Chemical abundances of Seyfert 2 AGNs – I. Comparing oxygen abundances from distinct methods using SDSS
We compare the oxygen abundance (O/H) of the narrow-line regions (NLRs) of Seyfert 2 AGNs obtained through strong-line methods and from direct measurements of the electron temperature (Te-method).
An Updated Line List for NUV Spectral Synthesis in Evolved Stars: Redetermination of the Beryllium Abundance in the Solar Photosphere
Motivated by the desire to measure beryllium abundances in red giant stars, we have constructed a new line list for synthesizing spectra in the near-ultraviolet. Using the Sun, Arcturus, and Pollux
Optical and NIR spectroscopy of cool CEMP stars to probe the nucleosynthesis in low-mass AGB binary system
We present the abundance analyses of 7 Carbon enhanced metal-poor (CEMP) stars to understand the origin of carbon in them. We used high-resolution optical spectra to derive abundances of various
Ambient Column Densities of Highly Ionized Oxygen in Precipitation-limited Circumgalactic Media
  • G. Voit
  • Physics
    The Astrophysical Journal
  • 2019
Many of the baryons associated with a galaxy reside in its circumgalactic medium (CGM), in a diffuse volume-filling phase at roughly the virial temperature. Much of the oxygen produced over cosmic
Chemical composition of the solar surface
The Sun provides a standard reference against which we compare the chemical abundances found anywhere else in the Universe. Nevertheless, there is not a unique ‘solar’ composition, since the chemical
Hydrodynamical model atmospheres: Their impact on stellar spectroscopy and asteroseismology of late-type stars
Hydrodynamical, i.e. multi-dimensional and time-dependent, model atmospheres of late-type stars have reached a high level of realism. They are commonly applied in high-fidelity work on stellar
Reaching the Oldest Stars beyond the Local Group: Ancient Star Formation in UGC 4483
We present new WFC3/UVIS observations of UGC 4483, the closest example of a metal-poor blue compact dwarf galaxy, with a metallicity of Z ≃ 1/15 Z ⊙ and located at a distance of D ≃ 3.4 Mpc. The


The photospheric solar oxygen project. I. Abundance analysis of atomic lines and influence of atmosp
Context: The solar oxygen abundance has undergone a major downward revision in the past decade, the most noticeable one being the update including 3D hydrodynamical simulations to model the solar
The photospheric solar oxygen project: II. Non-concordance of the oxygen abundance derived from two forbidden lines
In the Sun, the two forbidden [OI] lines at 630 and 636 nm were previously found to provide discrepant oxygen abundances. aims: We investigate whether this discrepancy is peculiar to the Sun or
Determinations of the solar oxygen content relying on the neutral forbidden transition at 630 nm depend upon the nickel abundance, due to a Ni i blend. Here, we rederive the solar nickel abundance,
Line formation in solar granulation IV. (O I), O I and OH lines and the photospheric O abundance
The solar photospheric oxygen abundance has been determined from (O I), O I, OH vibration-rotation and OH pure rotation lines by means of a realistic time-dependent, 3D, hydrodynamical model of the
Oxygen lines in solar granulation. II. Centre-to-limb variation, NLTE line formation, blends, and th
Context. There is a lively debate about the solar oxygen abundance and the role of 3D models in its recent downward revision. These models have been tested using high-resolution solar atlases of flux
Another forbidden solar oxygen abundance: the [O I] 5577 Å line
Context. Recent works with improved model atmospheres, line formation, atomic and molecular data, and detailed treatment of blends have resulted in a significant downward revision of the solar oxygen
Solar Forbidden Oxygen, Revisited
Recent large reductions in the solar oxygen abundance, based on synthesis of photospheric O I, OH, and CO absorptions with 3D convection models, have provoked consternation in the helioseismology
Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere
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
The Solar Oxygen Crisis: Probably Not the Last Word
In this work we present support for recent claims that advocate a downward revision of the solar oxygen abundance. Our analysis employs spatially resolved spectropolarimetric observations including
The Solar Oxygen Abundance from an Empirical Three-Dimensional Model
The Oxygen abundance in the solar photosphere, and consequently the solar metallicity itself, is still a controversial issue with far-reaching implications in many areas of Astrophysics. This paper