Detailed chemical compositions of the wide binary HD 80606/80607: revised stellar properties and constraints on planet formation

Liu, F.; Yong, David; Asplund, Martin; Feltzing, Sofia; Mustill, Alexander J.; Meléndez, Jorge; Ramírez, Iván; Lin, Jane

doi:10.1051/0004-6361/201832701

Cited by 36 publications

(26 citation statements)

References 83 publications

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“…One should not be misled by the selection of examples above to believe that all solar-type binary stars show pronounced abundance differences scaling with condensation temperatures. One example of the contrary is the wide system HD80606/ 80607 where the two components were found in a high-precision analysis by Liu et al (2018) to depart in metallicity by 0.013 ±0.002 dex (!) but with no clear variation with condensation temperature.…”

Section: Binariesmentioning

confidence: 99%

High-precision stellar abundances of the elements: methods and applications

Nissen

Gustafsson

2018

Astron Astrophys Rev

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Efficient spectrographs at large telescopes have made it possible to obtain high-resolution spectra of stars with high signal-to-noise ratio and advances in model atmosphere analyses have enabled estimates of high-precision differential abundances of the elements from these spectra, i.e. with errors in the range 0.01 -0.03 dex for F, G, and K stars.Methods to determine such high-precision abundances together with precise values of effective temperatures and surface gravities from equivalent widths of spectral lines or by spectrum synthesis techniques are outlined, and effects on abundance determinations from using a 3D non-LTE analysis instead of a classical 1D LTE analysis are considered.The determination of high-precision stellar abundances of the elements have led to the discovery of unexpected phenomena and relations with important bearings on the astrophysics of galaxies, stars, and planets, i.e. i) Existence of discrete stellar populations within each of the main Galactic components (disk, halo, and bulge) providing new constraints on models for the formation of the Milky Way. ii) Differences in the relation between abundances and elemental condensation temperature for the Sun and solar twins suggesting dust-cleansing effects in proto-planetary disks and/or engulfment of planets by stars; iii) Differences in chemical composition between binary star components and between members of open or globular clusters showing that star-and cluster-formation processes are more complicated than previously thought; iv) Tight relations between some abundance ratios and age for solar-like stars providing new constraints on nucleosynthesis and Galactic chemical evolution models as well as the composition of terrestrial exoplanets.We conclude that if stellar abundances with precisions of 0.01 -0.03 dex can be achieved in studies of more distant stars and stars on the giant and supergiant branches, many more interesting future applications, of great relevance to stellar and galaxy evolution, are probable. Hence, in planning abundance surveys, it is important to carefully balance the need for large samples of stars against the spectral resolution and signal-to-noise ratio needed to obtain high-precision abundances. Furthermore, it is an advantage to work differentially on stars with similar atmospheric parameters, because then a simple 1D LTE analysis of stellar spectra may be sufficient. However, when determining high-precision absolute abundances or differential abundance between stars having more widely different parameters, e.g. metal-poor stars compared to the Sun or giants to dwarfs, then 3D non-LTE effects must be taken into account.

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Section: Binariesmentioning

confidence: 99%

High-precision stellar abundances of the elements: methods and applications

Nissen

Gustafsson

2018

Astron Astrophys Rev

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“…Albeit no differences have been found in HAT-P-1 (Liu et al 2014), HD 80606/HD 80607 (Saffe et al 2015;Mack et al 2016), and HD 20782/HD 20781 (Mack et al 2014) and HD 106515 (Saffe et al 2019), the evidence is inconclusive in the latter three as a consequence of high abundance errors. Indeed, a more precise abundance analysis of the pair HD 80606/HD 80607 by Liu et al (2018) shows small but detectable abundance differences between the binary components. HD 240429/HD 240430 is a binary system of twin stars with large abundance differences (Oh et al 2018), for which no planets are known yet.…”

Section: Introductionmentioning

confidence: 99%

Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances

Maia

Meléndez

Lorenzo-Oliveira

et al. 2019

A&A

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The binary system 16 Cygni is key in studies of the planet-star chemical composition connection, as only one of the stars is known to host a planet. This allows us to better assess the possible influence of planet interactions on the chemical composition of stars that are born from the same cloud and thus should have a similar abundance pattern. In our previous work, we found clear abundance differences for elements with Z ≤ 30 between both components of this system and a trend of these abundances as a function of the condensation temperature (Tc), which suggests a spectral chemical signature related to planet formation. In this work we show that our previous findings are still consistent even if we include more species, such as the volatile N and neutron capture elements (Z > 30). We report a slope with Tc of 1.56 ± 0.24 × 10−5 dex K−1, that is good agreement with our previous work. We also performed some tests using ARES and iSpec to measure automatically the equivalent width and found Tc slopes in reasonable agreement with our results as well. In addition, we determined abundances for Li and Be by spectral synthesis, finding that 16 Cyg A is richer not only in Li but also in Be, when compared to its companion. This may be evidence of planet engulfment, indicating that the Tc trend found in this binary system may be a chemical signature of planet accretion in the A component, rather than an imprint of the giant planet rocky core formation on 16 Cyg B.

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“…They tentatively attributed the large abundance differences to the effects of planet engulfment. Furthermore, subtle or moderate abundance differences ( ∼ < 0.03 dex) without clear T cond trend were reported in several binary systems (e.g., WASP-94 A/B, HD 133131A/B, HD 106515A/B, HD 20781/20782, HAT-P-1 system and HD 80606/07) by Teske, Khanal & Ramírez (2016a), Teske et al (2016b, hereafter T16), Saffe et al (2019, hereafter S19), Mack et al (2014), Liu et al (2014) and Liu et al (2018), respectively. These studies may demonstrate that hosting close-in giant planets does not necessarily alter the stellar surface abundances, although no conclusive interpretation was offered.…”

Section: Introductionmentioning

confidence: 79%

Detailed elemental abundances of binary stars: Searching for signatures of planet formation and atomic diffusion

Liu,

Bitsch,

Asplund

et al. 2021

Preprint

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Binary star systems are assumed to be co-natal and coeval, thus to have identical chemical composition. In this work we aim to test the hypothesis that there is a connection between observed element abundance patterns and the formation of planets using binary stars. Moreover, we also want to test how atomic diffusion might influence the observed abundance patterns. We conduct a strictly line-by-line differential chemical abundance analysis of 7 binary systems. Stellar atmospheric parameters and elemental abundances are obtained with extremely high precision (< 3.5%) using the high quality spectra from VLT/UVES and Keck/HIRES. We find that 4 of 7 binary systems show subtle abundance differences (0.01 -0.03 dex) without clear correlations with the condensation temperature, including two planet-hosting pairs. The other 3 binary systems exhibit similar degree of abundance differences correlating with the condensation temperature. We do not find any clear relation between the abundance differences and the occurrence of known planets in our systems. Instead, the overall abundance offsets observed in the binary systems (4 of 7) could be due to the effects of atomic diffusion. Although giant planet formation does not necessarily imprint chemical signatures onto the host star, the differences in the observed abundance trends with condensation temperature, on the other hand, are likely associated with diverse histories of planet formation (e.g., formation location). Furthermore, we find a weak correlation between abundance differences and binary separation, which may provide a new constraint on the formation of binary systems.

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Detailed chemical compositions of the wide binary HD 80606/80607: revised stellar properties and constraints on planet formation

Cited by 36 publications

References 83 publications

High-precision stellar abundances of the elements: methods and applications

High-precision stellar abundances of the elements: methods and applications

Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances

Detailed elemental abundances of binary stars: Searching for signatures of planet formation and atomic diffusion

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