Sulfur Abundances in Metal-Poor Stars Based on OAO-1.88m/HIDES Spectra

Details Sulfur Abundances in Metal-Poor Stars Based on OAO-1.88m/HIDES Spectra Sulfur Abundances in Metal-Poor Stars Based on OAO-1.88m/HIDES Spectra

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005pasj...57..347t&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.57, No.2, pp. 347-363

Astronomy and Astrophysics

Astronomy

10

Galaxy: Evolution, Stars: Abundances, Stars: Population Ii, Stars: Sulfur

Scientific paper

The LTE abundances of sulfur (S) of 21 metal-poor stars and one normal star were explored in the metallicity range of -3 < [Fe/H] ≤ 0, based on the equivalent widths of the S I (1) 9212, 9237Å and S I (6) 8693, 9894Å lines measured on high-resolution spectra, which were observed by the OAO 1.88-m telescope equipped with HIDES. Our main results are: (1) The abundances derived from the S I (6) lines are consistent with those from the S I (1) lines among our sample stars in the range of [Fe/H] > -2 with an average difference of +0.03 ± 0.05 dex, whereas a significant discrepancy is observed in the range of [Fe/H] ≤ -2. (2) The behavior of [S(6)/Fe], versus [Fe/H] of our halo sample stars exhibits a nearly flat trend with an average of +0.62 ± 0.09 dex in the range of -3 < [Fe/H] < -1.25, and shows a distribution around +0.29 dex in -1.25 ≤ [Fe/H] ≤ -0.7. Our sample stars with -1.25 ≤ [Fe/H] ≤ -0.5 follow an increasing trend with decreasing [Fe/H]. The behavior of [S(1)/Fe] of our sample stars also shows essentially the same trend as [S(6)/Fe], though it is quantitatively different. (3) The S behavior in the range of -3 < [Fe/H] ≤ 0 inferred from the abundances of multiplets 6 and 1 are qualitatively consistent with each other, and may be represented by a combination of a nearly flat trend and a linearly increasing trend with decreasing [Fe/H]. A transition of the trend is likely to occur at [Fe/H] ˜ -1.5 dex.

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