C3PO – IV. Co-natal stars depleted in refractories are magnetically more active – possible imprints of planets
Article
Article Title | C3PO – IV. Co-natal stars depleted in refractories are magnetically more active – possible imprints of planets |
---|---|
ERA Journal ID | 1074 |
Article Category | Article |
Authors | Yu, Jie, Ting, Yuan-Sen, Casagrande, Luca, Liu, Fan, Wang, Sharon X, Sun, Qinghui, Huber, Daniel, Chen, Boquan, Cordoni, Giacomo, Da Costa, Gary, Huang, Chelsea X, Karakas, Amanda I, Khanna, Shourya, Zhu, Junhui, Ness, Melissa K., Nordlander, Thomas and Taylor, Taylor |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 538 (4), pp. 2408-2420 |
Number of Pages | 13 |
Year | 2025 |
Publisher | Oxford University Press |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/staf436 |
Web Address (URL) | https://academic.oup.com/mnras/article/538/4/2408/8082124 |
Abstract | Chemical abundance anomalies in twin stars have recently been considered tell-tale signs of interactions between stars and planets. While such signals are prevalent, their nature remains a subject of debate. On the one hand, exoplanet formation may induce chemical depletion in host stars by locking up refractory elements. On the other hand, exoplanet engulfment can result in chemical enrichment, and both processes potentially produce similar differential signals. In this study, we aim to observationally disentangle these processes by using the Ca ii infrared triplet to measure the magnetic activity of 125 co-moving star pairs with high signal-to-noise ratio, and high-resolution spectra from the Magellan, Keck, and VLT (Very Large Telescope) telescopes. We find that co-natal star pairs in which the two stars exhibit significant chemical abundance differences also show differences in their magnetic activity, with stars depleted in refractories being magnetically more active. Furthermore, the strength of this correlation between differential chemical abundances and differential magnetic activity increases with condensation temperature. One possible explanation is that the chemical anomaly signature may be linked to planet formation, wherein refractory elements are locked into planets, and the host stars become more active due to more efficient contraction during the pre-main-sequence phase or star–planet tidal and magnetic interactions. |
Keywords | planets and satellites: formation; stars: rotation; stars: activity; stars: abundances |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Byline Affiliations | Australian National University |
Ohio State University, United States | |
Max Planck Institute for Astronomy, Germany | |
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia | |
Monash University | |
Tsinghua University, China | |
Shanghai Jiao Tong University, China | |
University of Hawaii, United States | |
University of Sydney | |
Centre for Astrophysics | |
INAF - Astrophysical Observatory of Turin, Italy | |
Xiamen University, China | |
Columbia University, United States | |
Flatiron Institute, United States | |
Uppsala University, Sweden |
https://research.usq.edu.au/item/zx214/c3po-iv-co-natal-stars-depleted-in-refractories-are-magnetically-more-active-possible-imprints-of-planets
Download files
43
total views3
total downloads22
views this month2
downloads this month