English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

CONTEXT: In recent years, the solar chemical abundances have been studied inconsiderable detail because of discrepant values of solar metallicity inferredfrom different indicators, i.e., on the one hand, the "sub-solar" photosphericabundances resulting from spectroscopic chemical composition analyses with theaid of 3D hydrodynamical models of the solar atmosphere, and, on the otherhand, the high metallicity inferred by helioseismology. AIMS: Afterinvestigating the solar oxygen abundance using a CO5BOLD 3D hydrodynamicalsolar model in previous work, we undertake a similar approach studying thesolar abundance of nitrogen, since this element accounts for a significantfraction of the overall solar metallicity, Z. METHOD: We used a selection ofatomic spectral lines to determine the solar nitrogen abundance, relying mainlyon equivalent width measurements in the literature. We investigate theinfluence on the abundance analysis, of both deviations from localthermodynamic equilibrium ("NLTE effects") and photospheric inhomogeneities("granulation effects"). RESULTS: We recommend use of a solar nitrogenabundance of A(N)=7.86+-0.12 whose error bar reflects the line-to-line scatter.CONCLUSION: The solar metallicity implied by the CO5BOLD-based nitrogen andoxygen abundances is in the range 0.0145<= Z <= 0.0167. This result is a steptowards reconciling photospheric abundances with helioseismic constraints on Z.Our most suitable estimates are Z=0.0156 and Z/X=0.0213.

The solar photospheric nitrogen abundance. Analysis of atomic transitions with 3D and 1D model atmospheres