ELEMENTAL ABUNDANCES OF SOLAR SIBLING CANDIDATES

被引：26

作者：

Ramirez, I. ^{[1
,2
]}

Bajkova, A. T. ^{[3
]}

Bobylev, V. V. ^{[3
,4
]}

Roederer, I. U. ^{[5
]}

Lambert, D. L. ^{[1
,2
]}

Endl, M. ^{[1
,2
]}

Cochran, W. D. ^{[1
,2
]}

MacQueen, P. J. ^{[1
,2
]}

Wittenmyer, R. A. ^{[6
,7
]}

机构：

[1] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA

[2] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[3] RAS, Cent Pulkovo Astron Observ, St Petersburg 196140, Russia

[4] St Petersburg State Univ, Sobolev Astron Inst, St Petersburg 198504, Russia

[5] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[6] UNSW Australia, Sch Phys, Sydney, NSW 2052, Australia

[7] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 787卷 / 02期

基金：

美国国家科学基金会;

关键词：

stars: abundances; stars: fundamental parameters; stars: general; stars: individual (HD 162826); stars: kinematics and dynamics; GENEVA-COPENHAGEN SURVEY; METAL-POOR STARS; LABORATORY TRANSITION-PROBABILITIES; PLANET SEARCH PROGRAM; R-PROCESS-RICH; STELLAR EVOLUTION DATABASE; OPEN CLUSTERS; BARIUM STARS; G-DWARF; CHEMICAL EVOLUTION;

D O I：

10.1088/0004-637X/787/2/154

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Dynamical information along with survey data on metallicity and in some cases age have been used recently by some authors to search for candidates of stars that were born in the cluster where the Sun formed. We have acquired high-resolution, high signal-to-noise ratio spectra for 30 of these objects to determine, using detailed elemental abundance analysis, if they could be true solar siblings. Only two of the candidates are found to have solar chemical composition. Updated modeling of the stars' past orbits in a realistic Galactic potential reveals that one of them, HD 162826, satisfies both chemical and dynamical conditions for being a sibling of the Sun. Measurements of rare-element abundances for this star further confirm its solar composition, with the only possible exception of Sm. Analysis of long-term high-precision radial velocity data rules out the presence of hot Jupiters and confirms that this star is not in a binary system. We find that chemical tagging does not necessarily benefit from studying as many elements as possible but instead from identifying and carefully measuring the abundances of those elements that show large star-to-star scatter at a given metallicity. Future searches employing data products from ongoing massive astrometric and spectroscopic surveys can be optimized by acknowledging this fact.

引用

页数：17