TY - JOUR
T1 - Planets Around Solar Twins/Analogs (PASTA). I. High-precision Stellar Chemical Abundances for 17 Planet-hosting Stars and the Condensation Temperature Trend
AU - Sun, Qinghui
AU - Wang, Sharon Xuesong
AU - Gan, Tianjun
AU - Ji, Chenyang
AU - Lin, Zitao
AU - Ting, Yuan Sen
AU - Teske, Johanna
AU - Li, Haining
AU - Liu, Fan
AU - Hua, Xinyan
AU - Tang, Jiaxin
AU - Yu, Jie
AU - Zhang, Jiayue
AU - Badenas-Agusti, Mariona
AU - Vanderburg, Andrew
AU - Ricker, George R.
AU - Vanderspek, Roland
AU - Latham, David W.
AU - Seager, Sara
AU - Jenkins, Jon M.
AU - Schwarz, Richard P.
AU - Guillot, Tristan
AU - Tan, Thiam Guan
AU - Conti, Dennis M.
AU - Collins, Kevin I.
AU - Srdoc, Gregor
AU - Stockdale, Chris
AU - Suarez, Olga
AU - Zambelli, Roberto
AU - Radford, Don
AU - Barkaoui, Khalid
AU - Evans, Phil
AU - Bieryla, Allyson
N1 - Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.
PY - 2025/2/20
Y1 - 2025/2/20
N2 - 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]solar-[X/Fe]star) versus condensation temperature (Tc) 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 the solar-like stars, we find that all stars hosting known gas giant planets exhibit negative Tc trend slopes, suggesting that the Sun is relatively depleted in refractory elements compared to similar giant planet-hosting stars. Additionally, we find no correlation between Tc 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.
AB - 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]solar-[X/Fe]star) versus condensation temperature (Tc) 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 the solar-like stars, we find that all stars hosting known gas giant planets exhibit negative Tc trend slopes, suggesting that the Sun is relatively depleted in refractory elements compared to similar giant planet-hosting stars. Additionally, we find no correlation between Tc 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.
UR - http://www.scopus.com/inward/record.url?scp=85218970917&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ad9924
DO - 10.3847/1538-4357/ad9924
M3 - Article
AN - SCOPUS:85218970917
SN - 0004-637X
VL - 980
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 179
ER -