Abstract
The solar abundance of iron is determined from strong lines of Fe I with well-determined f-values using collision-damping constants for the lines from the theory of Anstee & O'Mara. The derived abundance is independent of non-thermal motions in the solar photosphere and is in excellent agreement with the meteoritic abundance of iron. The results are discussed in the light of recent determinations of the abundance based on medium-strong lines of Fe I which have been a subject of some controversy. The results are also used to assess the accuracy of the line-broadening theory.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
