Abundance analysis of neodymium in the solar atmosphere
Request PDF | Abundance analysis of neodymium in the solar atmosphere | Based on non-local thermodynamical equilibrium (NLTE) calculations, the solar neodymium
The solar carbon, nitrogen, and oxygen abundances from a 3D
the helium abundance of the solar envelope and the location of the bottom of the convection zone). The former approach is model-insensitive; in contrast, the latter approach depends
Abundance analysis of neodymium in the solar atmosphere
The HM model is the favoured model of solar abundance analysis; owing to its temperature stratification, it is expected to be an accurate representation of the real
Abundances of Elements in Solar Systems
Their analysis also showed that exoplanets with exotic compositions, e.g., mantles made of albite, corundum, rutile, clinopyroxene, or garnet, may be incredibly rare, if
The solar lithium abundance | Solar Physics
The solar abundance of lithium and its isotopic abundance ratio were determined by comparing synthetic spectra with the high quality center-to-limb spectra of the solar lithium feature
M giants with IGRINS
The abundance trends for Mg, Si, S, and Ca are shown in Figs. 2–5, respectively, with the trends from each individual line in the top panels and the mean abundance estimated from all lines in
The solar photospheric nitrogen abundance
undertake a similar approach studying the solar abundance of nitrogen, since this element accounts for a significant fraction of the overall solar metallicity, Z. Methods.We used a
Differences in elemental abundances between CI chondrites and
We calculate these differences as (CI/P−1) i or (CI/G−1) i where CI, P, and G represent the CI chondrite abundance (Lodders 2021), the photospheric abundance (Asplund
The LTE solar abundance of silicon
THE LTE SOLAR ABUNDANCE OF NEODYMIUM A.G. A. Abdelkawy, A.M.K. Shaltout, M.M. Beheary and A. Bakry Department of Astronomy and Meteorology, Faculty of Science, Al
the application of classical spectrum synthesis to the
Solar abundances play a key role in astrophysics as they are the abundances relative to which all others are measured. Opacity is determined in metal-rich objects by the iron abundance and
The solar abundance of beryllium
Figure 4: Solar disc-integrated flux spectrum in the vicinity of the Beii absorption lines. A fit with LTE and non-LTE models are shown, where A(Be) = 1.32 is assumed. Taken fromKorotin &
Relative Atomic Solar System Abundances, Mass
This brief special communications article gives data for atomic abundances and mass fractions for the elemental and isotopic solar system composition, the atomic masses of the elements and their isotopes, the
The solar system Fe/Mg ratio
Here, we report analyses of Fe/Mg; the fluence ratio is shown to be equal to the solar abundance ratio. Fe is an important rock-forming element and of high cosmochemical
Solar Elemental Abundances
Solar elemental abundances, or solar system elemental abundances refer to the complement of chemical elements in the entire solar system. The sun contains more than 99-percent of the
The solar photospheric nitrogen abundance. Analysis of atomic
CONTEXT: In recent years, the solar chemical abundances have been studied in considerable detail because of discrepant values of solar metallicity inferred from different
The solar photospheric nitrogen abundance
Astronomy & Astrophysics (A&A) is an international journal which publishes papers on all aspects of astronomy and astrophysics
Abundance analysis of neodymium in the solar atmosphere
A comparison of the NLTE abundance corrections with the standard LTE analysis, log ϵPr(LTE) = 0.74 ± 0.08, reveals a positive correction of +0.01 dex, estimated from
Helium Abundance of the Sun: A Spectroscopic Analysis
To validate the adopted solar parameters, an abundance analysis was performed on the observed solar photospheric spectrum. Neutral and singly ionized absorption
High-resolution abundance analysis of HD 140283 | Astronomy
The abundance analysis provided an extensive line list suitable for metal-poor subgiant stars. The results for Li, CNO, α-, and iron peak elements are in good agreement with literature. The
The solar beryllium abundance revisited with 3D non-LTE models
The initial abundance was taken to be A(Be) init = 1.32 ± 0.04 based on the CI chondrite Orgueil and converted to the solar scale using silicon, magnesium, and iron and
Abundance analysis of the neodymium in the solar atmosphere
The solar Nd abundance has been revised over the past decades under the LTE treatment. Maier & Whaling (1977) were derived the Nd An abundance analysis in cool A and Ap stars based
Solar oxygen abundance | Monthly Notices of the Royal
The diagnostic O lines used in the abundance analysis are the triplet O i lines at 777 nm and the forbidden [O i] line at 630 nm (Table 1).The former lines arise in electric dipole
Solar Abundance Problem
Different methods have been developed to determine solar abundances. They include empirical, semi-empirical, and theoretical methods. The former two subclasses refer to
The abundance of silicon in the solar atmosphere
A re-analysis of the departures from LTE using 1D solar model atmospheres have revealed only the mean non-LTE silicon abundance correction with respect to standard
Solar Abundances: Measurements from Solar Spectroscopy and
Why solar abundance n A fundamental benchmark to normalize elemental abundance of almost all astronomical objects. n Planets: abundance of heavy elements is a crucial parameter to
Chemical abundance analysis of the open clusters Berkeley 32,
3.2. Abundance analysis. Abundance calculations and spectral synthesis (for oxygen) were performed using the latest version of the abundance calculation code originally described by
The Chemical Composition of the Sun
Extracting information about the Sun''s chemical composition from the solar spectrum requires realistic models of the solar atmosphere and the line-formation process. Traditional solar and
Martin Asplund arXiv:0909.0948v1 [astro-ph.SR] 4 Sep 2009
2 INGREDIENTS FOR SOLAR ABUNDANCE ANALYSIS 2.1 Observations Analyses of the solar photospheric chemical composition make use of the ele-mental fingerprints present in the
Solar Abundance Problem
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
On the solar abundance of indium
Abstract. The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical
The solar carbon, nitrogen, and oxygen abundances from a 3D LTE
The abundance values advocated in Sect. 3.3 generally agree well with those of Asplund et al. (2009), which was an updated analysis of Asplund et al. (2005b) for carbon and
6 FAQs about [Solar abundance analysis]
How is solar O abundance determined?
The solar O abundance can be inferred from a number of different atomic and molecular indicators (Table 3).
Why do we need to know the elemental abundances of the Sun?
Context. The chemical composition of the Sun is a fundamental yardstick in astronomy, relative to which essentially all cosmic objects are referenced. As such, having accurate knowledge of the solar elemental abundances is crucial for an extremely broad range of topics. Aims.
Are solar abundances a basis for chemical composition?
Present-day and proto-solar Solar System abundances With the Sun providing > 99.85% of the total mass in the Solar System, we can safely adopt the solar abundances as the basis of the chemical composition of the solar system overall.
What are photospheric abundances?
The photospheric abundances are certainly not without shortcomings themselves. While often referred to as observed elemental abundances, the chemical composition of the Sun cannot be directly measured from the observed solar spectrum.
How many spectroscopic abundance sets are there?
Currently there are two abundance sets to be considered, depending on which solar model atmospheres were used in the evaluation of spectroscopic observations. One set in Table 2 uses traditional 1D solar atmospheric models, the other set uses 3D atmospheric models, which contain more detailed descriptions of the physic in the solar atmosphere.
What is the recommended solar photospheric V abundance?
Vanadium (Z = 23). The recommended solar photospheric V abundance of Scott et al. (2015a) was based on a 3D LTE analysis of V I lines with an ad hoc non-LTE correction of 0.10 dex across the board in the absence of actual statistical equilibrium calculations based on the behaviour of Sc and Ti in 1D model atmospheres.