Comparison of elemental abundances from the literature and this work (filled circles) for the same stars. The y-axis shows the difference in abundance, [X/H]literature – [X/H]this work, plotted against the Tc of each element on the x-axis. Potassium (K) is excluded as it was not reported in the literature. The open squares and downward triangles show a direct comparison of abundances measured from HARPS and MIKE spectra using the same spectral lines and analysis methods applied in this study. The differences reflect both instrumental systematics and manual measurement variability between HARPS and MIKE. — astro-ph.EP
Context. Previous studies have suggested that the Sun is relatively depleted in refractory elements compared to other solar twins or analogs, potentially as a result of planet formation. However, such conclusions are often limited by inhomogeneous samples and a lack of direct comparison with stars known to host planets.
Aims. We aim to perform a homogeneous and precise abundance analysis of solar twins and analogs that host planets, to investigate possible chemical signatures associated with planet formation.
Methods. We obtain high-resolution, high signal-to-noise ratio Magellan/MIKE spectra for 25 solar-like stars, including 22 confirmed or candidate planet hosts and three comparison stars. Stellar parameters and elemental abundances for 23 elements (from C to Eu) are derived through a strict line-by-line differential analysis relative to the Sun.
Results. Our sample spans [Fe/H] = -0.23 to +0.18 dex and includes 20 solar analogs, six of which are solar twins. Typical abundance uncertainties range from 0.01 to 0.05 dex for lighter elements (e.g., Fe, Si, C, O, Na) and up to 0.1 dex for neutron-capture elements. The Sun is consistently depleted in refractory elements relative to all solar analogs and twins, regardless of planet type. Stars hosting small planets tentatively show slightly stronger refractory element depletion than those hosting giant planets, though the difference is not yet statistically significant.
Conclusions. We emphasize the need for strictly differential, line-by-line analyses relative to the Sun, as well as careful consideration of systematic differences between instruments, to ensure consistency and the homogeneity required to achieve our goals.
Qinghui Sun, Chenyang Ji, Sharon Xuesong Wang, Zitao Lin, Johanna Teske, Yuan-Sen Ting, Megan Bedell, Fan Liu
Comments: Main text has 9 pages, 3 figures, 4 tables; accepted for publication in A&A
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2508.06976 [astro-ph.EP] (or arXiv:2508.06976v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2508.06976
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Submission history
From: Qinghui Sun
[v1] Sat, 9 Aug 2025 13:13:19 UTC (1,200 KB)
https://arxiv.org/abs/2508.06976
Astrobiology,