Modeling Stellar Abundance Patterns Resulting from the Addition of Earth-like Planetary Material

Cowley, Charles R.; Bord, D. J.; Yüce, Kutluay

doi:10.3847/1538-3881/abdf5d

Cited by 12 publications

(7 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We refer to comprehensive theoretical studies concerning possible scenarios of planet formation and star-planet chemical composition relations, which try to incorporate and explain the observational results (e.g. Thiabaud et al 2015;Bitsch & Battistini 2020;Adibekyan et al 2021;Cowley et al 2021;Nibauer et al 2021;Schneider & Bitsch 2021;Schulze et al 2021, and references therein).…”

Section: Elemental Abundances Versus Condensation Temperaturesmentioning

confidence: 99%

“…Bedell et al 2018;Hinkel & Unterborn 2018;Adibekyan 2019;Cridland et al 2019;Bashi & Zucker 2022;Delgado Mena et al 2021;Kolecki & Wang 2021;Mishenina et al 2021); and elemental abundance versus condensation temperature (T c ) relations in planet-hosting stars (e.g. da Silva et al 2015;Bedell et al 2018;Liu et al 2020;Cowley et al 2021;Mishenina et al 2021). The large sample of homogeneously investigated comparison stars in our study allows to take into account spatial and temporal factors as well as other specificities of the Galactic and stellar evolution.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Chemical Composition Of Bright Stars In The Northern Hemisphere: Star-Planet Connection

Tautvaišienė,

Mikolaitis,

Drazdauskas

et al. 2022

Preprint

View full text Add to dashboard Cite

In fulfilling the aims of the planetary and asteroseismic research missions, such as that of the NASA Transiting Exoplanet Survey Satellite (TESS) space telescope, accurate stellar atmospheric parameters and a detailed chemical composition are required as input. We have observed high-resolution spectra for all 848 bright (V < 8 mag) stars that are cooler than F5 spectral class in the area up to 12 deg surrounding the northern TESS continuous viewing zone and uniformly determined the main atmospheric parameters, ages, orbital parameters, velocity components, and precise abundances of up to 24 chemical species (C(C 2 ), N(CN), [O

show abstract

Section: Elemental Abundances Versus Condensation Temperaturesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Chemical Composition Of Bright Stars In The Northern Hemisphere: Star-Planet Connection

Tautvaišienė,

Mikolaitis,

Drazdauskas

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…It is possible to relate the slopes of abundance vs 𝑇 c plots to an engulfed mass using the toy model of Cowley et al (2021) We assume solar abundances (Asplund et al 2021) for the mass and composition of the convection zone (SCZ) as well as the composition of the mass (𝑞 × 𝑀 BE ) added. Here, we take 𝑀 SCZ = 0.025𝑀 , having the Sun's composition (Asplund et al 2021).…”

Section: Solar Twins Condensation and Engulfmentmentioning

confidence: 99%

Galactic chemical evolution of the solar neighborhood, solar twins and exoplanet indicators

2022

Self Cite

View full text Add to dashboard Cite

Galactic chemical evolution (GCE), solar analogues or twins, and peculiarities of the solar composition with respect to the twins are inextricably related. We examine GCE parameters from the literature and present newly derived values using a quadratic fit that gives zero for a Solar age (i.e., 4.6 Gyr). We show how the GCE parameters may be used not only to "correct" abundances to the solar age, but to predict relative elemental abundances as a function of age. We address the question of whether the solar abundances are depleted in refractories and enhanced in volatiles and find that the answer is sensitive to the selection of a representative standard. The best quality data sets do not support the notion that the Sun is depleted in refractories and enhanced in volatiles. A simple model allows us to estimate the amount of refractory-rich material missing from the Sun or alternately added to the average solar twin. The model gives between zero and 1.4 earth masses.

show abstract

“…In the case of G 112-43/44, the ∆[X/H]-T cond trend in Fig. 4 could be due to sequestration of refractory elements (Meléndez et al 2009) in planets around G 112-44 or to accretion of earth-like material (Cowley et al 2021) into the convection zone of G 112-43. Alternative explanations include dust-gas separation in starforming clouds (Gustafsson 2018) or in proto-planetary disks (Booth & Owen 2020).…”

Section: Abundance Differences Between G 112-43 and G 112-44mentioning

confidence: 99%

G112-43/44: A metal-poor binary star with a unique chemical composition and kinematics like the Helmi streams

Nissen,

Silva-Cabrera,

Schuster

2021

Preprint

View full text Add to dashboard Cite

Context. Correlations between high-precision elemental abundance ratios and kinematics of halo stars provide interesting information about the formation and early evolution of the Galaxy. Aims. Element abundances of G 112-43/44, a metal-poor wide-orbit binary star with extreme kinematics, are revisited. Methods. High-precision studies of the chemical compositions of 94 metal-poor dwarf stars in the solar neighbourhood are used to compare abundance ratios for G 112-43/44 with ratios for stars having similar metallicity taking into account the effect of deviations from local thermodynamic equilibrium on the derived abundances, and Gaia EDR3 data are used to compare the kinematics. Results. The abundance ratios X/Fe of the two components of G 112-43/44 agree within ±0.05 dex for nearly all elements, but there is a hint of a correlation of the difference in [X/H] with elemental condensation temperature, which may be due to planet-star interactions. The Mg/Fe, Si/Fe, Ca/Fe, and Ti/Fe ratios of G 112-43/44 agree with the corresponding ratios for accreted (Gaia-Enceladus) stars, but Mn/Fe, Ni/Fe, Cu/Fe, and Zn/Fe are significantly enhanced with ∆ [Zn/Fe] reaching 0.25 dex. The kinematics show that G 112-43/44 belongs to the Helmi streams in the solar neighbourhood and in view of this, we discuss if the abundance peculiarities of G 112-43/44 can be explained by chemical enrichment from supernovae events in the progenitor dwarf galaxy of the Helmi streams. Interestingly, yields calculated for a helium shell detonation Type Ia supernova model can explain the enhancement of Mn/Fe, Ni/Fe, Cu/Fe, and Zn/Fe in G 112-43/44 and three other α-poor stars in the Galactic halo with abundances from the literature, one of which have Helmi streams kinematics. The helium shell detonation model predicts, however, also enhanced abundance ratios of Ca/Fe, Ti/Fe, and Cr/Fe in disagreement with the observed ratios.

show abstract

Modeling Stellar Abundance Patterns Resulting from the Addition of Earth-like Planetary Material

Cited by 12 publications

References 42 publications

Chemical Composition Of Bright Stars In The Northern Hemisphere: Star-Planet Connection

Chemical Composition Of Bright Stars In The Northern Hemisphere: Star-Planet Connection

Galactic chemical evolution of the solar neighborhood, solar twins and exoplanet indicators

G112-43/44: A metal-poor binary star with a unique chemical composition and kinematics like the Helmi streams

Contact Info

Product

Resources

About