Kavli Affiliate: Andrew Vanderburg
| First 5 Authors: Qinghui Sun, Sharon Xuesong Wang, Tianjun Gan, Chenyang Ji, Zitao Lin
| Summary:
The Sun is depleted in refractory elements compared to nearby solar twins,
which may be linked to the formation of giant or terrestrial planets. Here we
present high-resolution, high signal-to-noise spectroscopic data for 17
solar-like stars hosting planets, obtained with Magellan II/MIKE, to
investigate whether this depletion is related to planet formation. We derive
stellar parameters, including stellar atmosphere, age, radius, mass, and
chemical abundances for 22 elements from carbon to europium through
line-by-line differential analysis. Our uncertainties range from 0.01 dex for
Fe and Si to 0.08 dex for Sr, Y, and Eu. By comparing the solar abundances to
those of the 17 stars, we investigate the differential abundance ([X/Fe]$_{rm
solar}$ – [X/Fe]$_{rm star}$) versus condensation temperature ($T_c$) trend.
In particular, we apply Galactic chemical evolution corrections to five solar
twins within the full sample. Our results conform to previous studies that the
Sun is relatively depleted in refractory compared to volatile elements. For
both five solar twins and the rest of solar-like stars, we find that all stars
hosting known gas giant planets exhibit negative $T_c$ trend slopes, suggesting
that the Sun is relatively depleted in refractory elements compared to similar
giant-planet-host stars. Additionally, we find no correlation between $T_c$
trend slopes and the total mass of detected terrestrial planets in each system,
suggesting that terrestrial planet formation may not be the cause of refractory
element depletion in the Sun.
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