| Texto completo | |
| Autor(es): |
Liu, F.
[1]
;
Yong, D.
[2]
;
Asplund, M.
[2]
;
Wang, H. S.
[3]
;
Spina, L.
[4, 5]
;
Acuna, L.
[6]
;
Melendez, J.
[7]
;
Ramirez, I.
[8]
Número total de Autores: 8
|
| Afiliação do(s) autor(es): | [1] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Melbourne, Vic 3122 - Australia
[2] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611 - Australia
[3] Swiss Fed Inst Technol, Inst Particle Phys & Astrophys, Wolfgang Pauli Str 27, CH-8093 Zurich - Switzerland
[4] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Melbourne, Vic 3800 - Australia
[5] ARC Ctr Excellence All Sky Astrophys Three Dimens, Melbourne, Vic - Australia
[6] Aix Marseille Univ, Lab Astrophys Marseille, F-13388 Marseille 13 - France
[7] Univ Sao Paulo, Dept Astron IAG USP, Rua Matao 1226, BR-05508900 Sao Paulo - Brazil
[8] Tacoma Community Coll, 6501 South 19th St, Tacoma, WA 98466 - USA
Número total de Afiliações: 8
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 495, n. 4, p. 3961-3973, JUL 2020. |
| Citações Web of Science: | 0 |
| Resumo | |
We present a line-by-line differential analysis of a sample of 16 planet-hosting stars and 68 comparison stars using high-resolution, high signal-to-noise ratio spectra gathered using Keck. We obtained accurate stellar parameters and high-precision relative chemical abundances with average uncertainties in T-eff, log g, {[}Fe/H], and {[}X/H] of 15 K, 0.034 cm S-2, 0.012 dex, and 0.025 dex, respectively. For each planet host, we identify a set of comparison stars and examine the abundance differences (corrected for Galactic chemical evolution effect) as a function of the dust condensation temperature, T-cond, of the individual elements. While we confirm that the Sun exhibits a negative trend between abundance and T-cond, we also confirm that the remaining planet hosts exhibit a variety of abundance-T(cond )trends with no clear dependence upon age, metallicity, or T-eff. The diversity in the chemical compositions of planet-hosting stars relative to their comparison stars could reflect the range of possible planet-induced effects present in these planet hosts, from the sequestration of rocky material (refractory poor) to the possible ingestion of planets (refractory rich). Other possible explanations include differences in the time-scale, efficiency and degree of planet formation, or inhomogeneous chemical evolution. Although we do not find an unambiguous chemical signature of planet formation among our sample, the high-precision chemical abundances of the host stars are essential for constraining the composition and structure of their exoplanets. (AU) | |
| Processo FAPESP: | 18/04055-8 - Espectroscopia de alta precisão: das primeiras estrelas aos planetas |
| Beneficiário: | Jorge Luis Melendez Moreno |
| Modalidade de apoio: | Auxílio à Pesquisa - Temático |