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J/A+A/347/348       Solar abundance of iron                   (Grevesse+, 1999)

The solar abundance of iron and the photospheric model Grevesse N., Sauval A.J. <Astron. Astrophys. 347, 348 (1999)> =1999A&A...347..348G (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Sun Keywords: Atomic data - Sun: abundances - Sun: photosphere Abstract: Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the analyses of Fe I lines and, to a lesser extent, of Fe II lines. Based on a set of 65 solar Fe I lines, with accurate transition probabilities as well as new accurate damping constants, we construct a new empirical photospheric model. We succeed to reconcile abundance results obtained from low and high excitation Fe I lines as well as from Fe II lines and derive a solar photospheric abundance of iron, AFe=7.50±0.05, which perfectly agrees with the meteoritic value. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 25 70 New photospheric model
See also: J/A+A/274/555 : Asymmetry of FeI lines in solar spectrum (Stathopoulou+ 1993) J/A+A/340/300 : Fe II oscillator strengths (Raassen+ 1998) J/A+AS/102/269 : Lab. and solar highly-excited levels of Fe I (Nave+ 1993) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 F6.3 --- logTau0 Logarithmic value of the optical depth at 500nm 8- 12 I5 K T Temperature 14- 19 F6.3 0.1Pa logPe Logarithmic value of the electron pressure (in dyne/cm2) 21- 25 F5.3 0.1Pa logPg Logarithmic value of the gas pressure (in dyne/cm2)
Acknowledgements: Joan Vandekerckhove
(End) Patricia Bauer [CDS] 17-Jun-1999
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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