On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars

被引:2
作者
Di Rocco, H. O. [1 ,2 ]
Cruzado, A. [3 ,4 ]
Marchiano, P. E. [3 ]
机构
[1] UNCPBA, Consejo Nacl Invest Cientif & Tecn CONICET, IFAS, Ctr Invest Fis & Ingn,Ctr Provinc Buenos Airs CIF, RA-7000 Buenos Aires, DF, Argentina
[2] Consejo Nacl Invest Cient Tecn CONICET, RA-1917 Buenos Aires, DF, Argentina
[3] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-52425 Buenos Aires, DF, Argentina
[4] Inst Astrofis Plata CONICET, RA-1900 Buenos Aires, DF, Argentina
来源
ASTRONOMY & ASTROPHYSICS | 2015年 / 581卷
关键词
atomic data; line: identification; stars: abundances; stars: chemically peculiar; SINGLY IONIZED XENON; 2ND SPECTRUM;
D O I
10.1051/0004-6361/201526301
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. The ultimate goal that has motivated this work is to achieve realistic oscillator strength (gf) values to find reliable values of stellar abundances. We aim to compare the gf values of Xe II lines found with different theoretical and experimental methods. Methods. We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare these results with those previously obtained from UVES spectra of HgMn stars. Results. 1) Our theoretical gf values are more realistic than those previously obtained for most lines. When we consider only unblended, isolated, relatively noise-free lines, however, our theoretical gf values and Yuce's stellar values differ little from each other. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xe II lines deducted from stellar spectra and those published by National Institute of Standards and Technology (NIST), we conclude that stellar wavelengths could be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 x 10(16) part. cm(-3).
引用
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页数:6
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