Experimental [CLC][ITAL]f[/ITAL][/CLC]-Value and Isotopic Structure for the N[CLC]i[/CLC] [CSC]i[/CSC] Line Blended with [O [CSC]i[/CSC]] at 6300 Å

Johansson, Sveneric; Litzén, Ulf; Lundberg, Hans; Zhang, Z

doi:10.1086/374037

Cited by 150 publications

(168 citation statements)

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“…We considered the two major isotopes 58 Ni i and 60 Ni i, with a log(gf) value of -2.11 and a fraction of 72% and 28% respectively for each isotope (Johansson et al (2003); see Table 1). …”

Section: Solar Model Used and Synthesismentioning

confidence: 99%

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Uncertainties in the solar photospheric oxygen abundance

Armas

Ramos

Socas‐Navarro

2017

A&A

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Aims. 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 Å, including correlations with other parameters involved. Methods. We worked with a three-dimensional empirical model and two solar intensity atlases. We employed Bayesian inference as a tool to determine the most probable value for the solar oxygen abundance given the model chosen. We considered a number of error sources, such as uncertainties in the continuum derivation, in the wavelength calibration and in the abundance/strength of Ni. Results. Our results shows correlations between the effects of several parameters employed in the derivation. The Bayesian analysis provides robust confidence limits taking into account all of these factors in a rigorous manner. We obtain that, given the empirical threedimensional model and the atlas observations employed here, the most probable value for the solar oxygen abundance is log( O ) = 8.86 ± 0.04. However, we note that this uncertainty does not consider possible sources of systematic errors due to the model choice.

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“…We considered the two major isotopes 58 Ni i and 60 Ni i, with a log(gf) value of -2.11 and a fraction of 72% and 28% respectively for each isotope (Johansson et al (2003); see Table 1). …”

Section: Solar Model Used and Synthesismentioning

confidence: 99%

“…The g f value used in this work (Johansson et al 2003) is accepted as the most accurate, but its uncertainty can go up to…”

Section: Abundance and Log(g F ) Factormentioning

confidence: 99%

Uncertainties in the solar photospheric oxygen abundance

Armas

Ramos

Socas‐Navarro

2017

A&A

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“…The Ni I line at 6300.34 Å was taken into account in the synthesis of the Oxygen line. For the Ni I line we adopted the log g f value derived by Johansson et al (2003), namely log g f = −2.11. The nitrogen abundance was derived by synthesis of the 8001−8005 Å spectral region, which is rich in CN lines.…”

Section: Chemical Abundance Analysismentioning

confidence: 99%

Lithium-rich giants in the Galactic thick disk

Monaco

Villanova

Bidin

et al. 2011

A&A

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Context. Lithium is a fragile element, which is easily destroyed in the stellar interior. The existence of lithium-rich giants still represents a challenge for stellar evolution models. Aims. We have collected a large database of high-resolution stellar spectra of 824 candidate thick-disk giants having 2 MASS photometry and proper motions measured by the Southern Proper-Motion Program (SPM). In order to investigate the nature of Li-rich giants, we searched this database for giants presenting a strong Li I resonance line. Methods. We performed a chemical abundance analysis on the selected stars with the MOOG code along with proper ATLAS-9 model atmospheres. The iron content and atmospheric parameters were fixed by using the equivalent width of a sample of Fe lines. We also derive abundances for C, N, and O and measure or derive lower limits on the 12 C/ 13 C isotopic ratios, which is a sensible diagnostic of the stars evolutionary status. Results. We detected five stars with a lithium abundance higher than 1.5, i.e. Li-rich according to the current definition. One of them (SPM-313132) has A(Li) > 3.3 and, because of this, belongs to the group of the rare super Li-rich giants. Its kinematics makes it a likely thin-disk member and its atmospheric parameters are compatible with it being a 4 M star either on the red giant branch (RGB) or the early asymptotic giant branch. This object is the first super Li-rich giant detected at this phase. The other four are likely low-mass thick-disk stars evolved past the RGB luminosity bump, as determined from their metallicities and atmospheric parameters. The most evolved of them lies close to the RGB-tip. It has A(Li) > 2.7 and a low 12 C/ 13 C isotopic ratio, close to the cool bottom processing predictions.

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“…The original line strength from the VALD database combined with the meteoritic Sc abundance yields a satisfactory fit to the line shape, as shown below. Oscillator strengths for the two relevant Ni isotopes (treated here as two blended lines with a slight wavelength shift) were adopted from Johansson et al (2003). The isotopes considered are 58 Ni and 60 Ni with 72% and 28% abundances, respectively.…”

Section: Observations and The Modelmentioning

confidence: 99%

The solar oxygen abundance from an empirical three-dimensional model

Socas‐Navarro

2015

A&A

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The oxygen abundance in the solar photosphere, and consequently the solar metallicity itself, is still a controversial question with farreaching implications in many areas of astrophysics. This paper presents a new determination obtained by fitting the forbidden O i line at 6300 Å with an observational 3D model. The approach presented here is novel because previous determinations were based either on 1D empirical stratifications or on 3D theoretical models. The resulting best-fit abundances are log (O) = 8.90 and log (Ni) = 6.15. Nevertheless, by introducing minor tweaks in the model and the procedure, it is possible to retrieve very different values, even down to log (O) = 8.70. This extreme sensitivity of the abundance to possible systematic effects is not specific to this particular work, but probably reflects the real uncertainty inherent to all abundance determinations based on a prescribed model atmosphere.

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Experimental [CLC][ITAL]f[/ITAL][/CLC]-Value and Isotopic Structure for the N[CLC]i[/CLC] [CSC]i[/CSC] Line Blended with [O [CSC]i[/CSC]] at 6300 Å

Cited by 150 publications

References 10 publications

Uncertainties in the solar photospheric oxygen abundance

Uncertainties in the solar photospheric oxygen abundance

Lithium-rich giants in the Galactic thick disk

The solar oxygen abundance from an empirical three-dimensional model

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