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The Chemical Composition of the Sun
The solar chemical composition is an important ingredient in our understanding of the formation, structure, and evolution of both the Sun and our Solar System. Furthermore, it is an essential referExpand
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 theExpand
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey
We present a re-analysis of the Geneva-Copenhagen survey, which benefits from the infrared flux method to improve the accuracy of the derived stellar effective temperatures and uses the latter toExpand
The Solar Chemical Composition
Abstract We present our current knowledge of the solar chemical composition based on the recent significant downward revision of the solar photospheric abundances of the most abundant metals. TheseExpand
New light on stellar abundance analyses: Departures from LTE and homogeneity.
▪ Abstract The information on the chemical compositions of stars encoded in their spectra plays a central role in contemporary astrophysics. Stellar element abundances are, however, not observed: toExpand
ARGOS - III. Stellar populations in the Galactic bulge of the Milky Way
We present the metallicity results from the ARGOS spectroscopic survey of the Galactic bulge. Our aim is to understand the formation of the Galactic bulge: did it form via mergers, as expected fromExpand
Nucleosynthetic signatures of the first stars
TLDR
The discovery of HE1327–2326 is reported, a subgiant or main-sequence star with an iron abundance about a factor of two lower than that of HE0107–5240, suggesting a similar origin of the abundance patterns. Expand
The chemical composition of the Sun
We present a redetermination of the solar abundances of all available elements. The new results have very recently been published by Asplund et al. (Annu. Rev. Astron. Astrophys. 47:481, 2009). TheExpand
A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3
TLDR
It is concluded that low-energy supernovae were common in the early Universe, and that suchsupernovae yielded light-element enrichment with insignificant iron. Expand
Non-LTE calculations for neutral Na in late-type stars using improved atomic data
Neutral sodium is a minority species in the atmospheres of late-type stars, and line formation in local thermodynamic equilibrium (LTE) is often a poor assumption, in particular for strong li nes. WeExpand
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