Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

Nibauer, Jacob; Baxter, Eric J.; Jain, Bhuvnesh; Saders, Jennifer L. van; Beaton, Rachael L.; Teske, Johanna

doi:10.3847/1538-4357/abd0f1

Cited by 8 publications

(20 citation statements)

References 66 publications

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“…Both the ASPCAP and predicted abundance distributions for the KOI and doppelgänger samples exhibit a tail of slopes toward the right of the distribution center that appears to peak at ∼4 × 10 −4 dex K −1 . A similar secondary peak was found by Nibauer et al (2021) in their T c slope distribution for >900 K elements from APOGEE DR16 data. This indicates that our data reproduce the T c patterns in field stars, which is reassuring.…”

Section: Condensation Temperature Trendssupporting

confidence: 81%

“…Elements are refractory rather than volatile above this temperature, and populate the steepest regions of abundance versus T c trends in patterns exhibiting refractory enhancement or depletion (Meléndez et al 2009;Ramírez et al 2009;Bedell et al 2018). This is similar to the analysis presented in Nibauer et al (2021), which assessed T c trends of elements with T c > 900 K. The resulting slope distributions for the predicted and ASPCAP abundances are shown in Figure 10. Both the ASPCAP and predicted abundance distributions for the KOI and doppelgänger samples exhibit a tail of slopes toward the right of the distribution center that appears to peak at ∼4 × 10 −4 dex K −1 .…”

Section: Condensation Temperature Trendssupporting

confidence: 71%

“…This indicates that our data reproduce the T c patterns in field stars, which is reassuring. However, we find fewer stars in the secondary peak at positive gradients compared to Nibauer et al (2021). This is potentially explained by our different stellar samples that span different evolutionary states; Nibauer et al (2021) examined stars across a narrow range of the main sequence whereas we study stars across the main sequence and red giant branch.…”

Section: Condensation Temperature Trendsmentioning

confidence: 70%

“…Such trends with T c have been observed in the differential abundances of several binary systems (Ramírez et al 2011;Mack et al 2014;Tucci Maia et al 2014;Biazzo et al 2015;Ramírez et al 2015;Teske et al 2015;Adibekyan et al 2016;Saffe et al 2016;Teske et al 2016;Saffe et al 2017;Oh et al 2018;Maia et al 2019;Ramírez et al 2019;Nagar et al 2020;Galarza et al 2021;Jofré et al 2021), and in larger samples. For example, Nibauer et al (2021) analyzed 1700 solar analogs from the Apache Point Galactic Evolution Experiment (APOGEE), and found that 70%−90% of solar analogs appear depleted in refractory elements in order of T c . Thus, there is ample evidence that abundance alteration via planet formation processes is common.…”

Section: Introductionmentioning

confidence: 99%

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Elemental Abundances of Kepler Objects of Interest in APOGEE DR17

Behmard

Ness

Cunningham

et al. 2023

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The elemental abundances of planet host stars can shed light on the conditions of planet forming environments. We test if individual abundances of 130 known/candidate planet hosts in APOGEE are statistically different from those of a reference doppelgänger sample. The reference set comprises objects selected with the same T eff, log g , [Fe/H], and [Mg/H] as each Kepler Object of Interest (KOI). We predict twelve individual abundances (X = C, N, O, Na, Al, Si, Ca, Ti, V, Cr, Mn, Ni) for the KOIs and their doppelgängers using a local linear model of these four parameters, training on ASPCAP abundance measurements for a sample of field stars with high-fidelity (signal-to-noise ratio > 200) APOGEE observations. We compare element prediction residuals (model–measurement) for the two samples and find them to be indistinguishable, given a high-quality sample selection. We report median intrinsic dispersions of ∼0.038 dex and ∼0.041 dex, for the KOI and doppelgänger samples, respectively, for these elements. We conclude that the individual abundances at fixed T eff, log g , [Fe/H], and [Mg/H] are unremarkable for known planet hosts. Our results establish an upper limit on the abundance precision required to uncover any chemical signatures of planet formation in planet host stars.

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Section: Condensation Temperature Trendssupporting

confidence: 81%

Section: Condensation Temperature Trendssupporting

confidence: 71%

Section: Condensation Temperature Trendsmentioning

confidence: 70%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Elemental Abundances of Kepler Objects of Interest in APOGEE DR17

Behmard

Ness

Cunningham

et al. 2023

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“…Is planet engulfment common or uncommon in solar twins is not yet clear (e.g. Nibauer et al 2021 ), suggesting the existence of two distinct populations. In Fig.…”

Section: An Empirical Model For Abundance As a Function Of Age And Me...mentioning

confidence: 99%

The GALAH Survey: dependence of elemental abundances on age and metallicity for stars in the Galactic disc

Sharma

Hayden

Bland-Hawthorn

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Using data from the GALAH survey, we explore the dependence of elemental abundances on stellar age and metallicity among Galactic disc stars. We find that the abundance of most elements can be predicted from age and [Fe/H] with an intrinsic scatter of about 0.03 dex. We discuss the possible causes for the existence of the abundance-age-metallicity relations. Using a stochastic chemical enrichment scheme that takes the volume of supernovae remnants into account, we show the intrinsic scatter is expected to be small, about 0.05 dex or even smaller if there is additional mixing in the ISM. Elemental abundances show trends with both age and metallicity and the relationship is well described by a simple model in which the dependence of abundance ([X/Fe]) on age and [Fe/H] are additively separable. Elements can be grouped based on the direction of their abundance gradient in the (age,[Fe/H]) plane and different groups can be roughly associated with three distinct nucleosynthetic production sites, the exploding massive stars, the exploding white dwarfs and the AGB stars. However, the abundances of some elements, like Co, La, and Li, show large scatter for a given age and metallicity, suggesting processes other than simple Galactic chemical evolution are at play. We also compare the abundance trends of main-sequence turn-off stars against that of giants, whose ages were estimated using asteroseismic information from the K2 mission. For most elements, the trends of main-sequence turn-off stars are similar to that of giants. The existence of abundance relations implies that we can estimate the age and birth radius of disc stars, which is important for studying the dynamic and chemical evolution of the Galaxy.

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The Star–Planet Composition Connection

Teske

2024

Annual Review of Astronomy and Astrophysics

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The mantra “know thy star, know thy planet” has proven to be very important for many aspects of exoplanet science. Here I review how stellar abundances inform our understanding of planet composition and, thus, formation and evolution. In particular, I discuss how: ▪ The strongest star–planet connection is still the giant planet–metallicity correlation, the strength of which may indicate a break point between the formation of planets versus brown dwarfs. ▪ We do not have very good constraints on the lower metallicity limit for planet formation, although new statistics from TESS are helping, and it appears that, at low [Fe/H], α elements can substitute for iron as seeds for planet formation. ▪ The depletion of refractory versus volatile elements in stellar photospheres (particularly the Sun) was initially suggested as a sign of small planet formation but is challenging to interpret, and small differences in binary star compositions can be attributed mostly to processes other than planet formation. ▪ We can and should go beyond comparisons of the carbon-to-oxygen ratio in giant planets and their host stars, incorporating other volatile and refractory species to better constrain planet formation pathways. ▪ There appears to be a positive correlation between small planet bulk density and host star metallicity, but exactly how closely small planet refractory compositions match those of their host stars—and their true diversity—is still uncertain.

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Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

Cited by 8 publications

References 66 publications

Elemental Abundances of Kepler Objects of Interest in APOGEE DR17

Elemental Abundances of Kepler Objects of Interest in APOGEE DR17

The GALAH Survey: dependence of elemental abundances on age and metallicity for stars in the Galactic disc

The Star–Planet Composition Connection

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