Stellar chemistry and planet size: Insights from GALAH DR4

The well-known correlation between stellar metallicity and the presence of planets is strongest for giant planets and weaker for smaller planets, suggesting that detailed elemental patterns beyond $ Fe / H $ may be relevant. Using abundances from the fourth data release of the GALAH spectroscopic survey, we analyzed 104 host stars with 141 confirmed transiting planets. We divided the planets at , the theoretical threshold radius above which planets are unlikely to be pure-water worlds. We find that large-planet hosts are enriched by mathord∼ 0.2,dex in iron and show a possible excess of highly volatile elements ( , , and ), though these measurements are affected by observational limitations, whereas small-planet hosts exhibit an enhanced contribution of the classical rock-forming elements ( , , , and ) relative to iron; this corresponds to a modest $ r_ p = 2.6,R_⊕ C N O Mg Si Ca Ti Rock / Fe $ offset of 0.06,dex, which is statistically significant, with a p value of 10^-4. These offsets remain significant for alternative radius cuts. A matched control sample of non-planet-host stars shows only weak and mostly statistically insignificant similar trends, confirming that the stronger chemical signatures are linked to the planetary characteristics. As our study relies on transiting planets, it mainly probes short-period systems (P<100,days). These results refine the planet–metallicity relation, highlighting the role of the relative balance between iron, volatiles, and rock-forming elements in planet formation.