Line formation in solar granulation: II. The photospheric Fe abundance

dc.contributor.authorAsplund, Martinen_US
dc.contributor.authorNordlund, Aen_US
dc.contributor.authorTrampedach, Ren_US
dc.contributor.authorStein, Robert Fen_US
dc.date.accessioned2002-12-10en_US
dc.date.accessioned2004-05-19T04:58:55Zen_US
dc.date.accessioned2011-01-05T08:30:04Z
dc.date.available2004-05-19T04:58:55Zen_US
dc.date.available2011-01-05T08:30:04Z
dc.date.created2000en_US
dc.date.issued2000en_US
dc.description.abstractThe solar photospheric Fe abundance has been determined using realistic ab initio 3D, time-dependent, hydrodynamical model atmospheres. The study is based on the excellent agreement between the predicted and observed line profiles directly rather than equivalent widths, since the intrinsic Doppler broadening from the convective motions and oscillations provide the necessary non-thermal broadening. Thus, three of the four hotly debated parameters (equivalent widths, microturbulence and damping enhancement factors) in the center of the recent solar Fe abundance dispute regarding Fe i lines no longer enter the analysis, leaving the transition probabilities as the main uncertainty. Both Fe i (using the samples of lines of both the Oxford and Kiel studies) and Fe ii lines have been investigated, which give consistent results: log epsilon_FeI = 7.44 +/- 0.05 and log epsilon_FeII = 7.45 +/- 0.10. Also the wings of strong Fe i lines return consistent abundances, log epsilon_FeII = 7.42 +/- 0.03, but due to the uncertainties inherent in analyses of strong lines we give this determination lower weight than the results from weak and intermediate strong lines. In view of the recent slight downward revision of the meteoritic Fe abundance log epsilon_Fe = 7.46 +/- 0.01, the agreement between the meteoritic and photospheric values is very good, thus appearingly settling the debate over the photospheric Fe abundance from Fe i lines.en_US
dc.format.extent495398 bytesen_US
dc.format.mimetypeapplication/pdfen_US
dc.identifier.urihttp://hdl.handle.net/1885/40078en_US
dc.identifier.urihttp://digitalcollections.anu.edu.au/handle/1885/40078
dc.language.isoen_AUen_US
dc.subjectconvectionen_US
dc.subjecthydronamicsen_US
dc.subjectline: formationen_US
dc.subjectsun: abundancesen_US
dc.subjectsun: granulationen_US
dc.subjectsun: photosphereen_US
dc.titleLine formation in solar granulation: II. The photospheric Fe abundanceen_US
dc.typeJournal articleen_US
local.description.refereedyesen_US
local.identifier.citationpages743-754en_US
local.identifier.citationpublicationAstronomy & Astrophysicsen_US
local.identifier.citationvolume359en_US
local.identifier.citationyear2000en_US
local.identifier.eprintid740en_US
local.rights.ispublishedyesen_US

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