Paper

An Ultra-Short Period Super-Earth and a Sub-Neptune Orbiting the K dwarf TOI-4311

Smith, Alexis M S, Rauer, Heike, Silva, André M, Scandariato, Gaetano, Venturini, Julia, Rando, Nicola, Brandeker, Alexis, Cubillos, Patricio E, Alain Lecavelier des Etangs, Ziegler, Carl, Alexander James Mustill, Baumjohann, Wolfgang, Heitzmann, Alexis, Yoshi Nike Emilia Eschen, Szabó, Gyula M, Deleuil, Magali, Wilson, Thomas G, Fridlund, Malcolm, Queloz, Didier, Lacedelli, Gaia, Derekas, Aliz, Piotto, Giampaolo, Isaak, Kate G, Barrado, David, Borsato, Luca, Santos, Nuno C, Brice-Olivier Demory, Magrin, Demetrio, Ségransan, Damien, Benz, Willy, Lam, Kristine W F, Ulmer, Bernd, Southworth, Richard, Kiss, Laszlo L, Akinsanmi, Babatunde, Ulmer-Moll, Solène, Barros, Susana C C, Bárczy, Tamas, Egger, Jo Ann, Bonfanti, Andrea, Demangeon, Olivier D S, Gandolfi, Davide, Deline, Adrien, Keller, Tatiana, Stalport, Manu, Ehrenreich, David, Csizmadia, Szilard, Correia, Alexandre C M, Pollacco, Don, Olofsson, Göran, Davies, Melvyn B, Ribas, Ignasi, Piazza, Daniele, Mordasini, Christoph, Adibekyan, Vardan, Jenkins, Jon M, Pezzotti, Camilla, Günther, Maximilian N, Gisbert, Peter, Giuseppe Di Persio, Fossati, Luca, Broe

2026

Overview

We report the discovery and characterisation of the multi-planetary system around TOI-4311, a K dwarf kinematically between the Galactic thick disk and Hercules stream. TOI-4311 hosts an ultra-short-period super-Earth (P\\(\\)0.99 d, \\(1.376+0.077\\\-0.080\\) R\\(_\\)) and a longer period sub-Neptune (P\\(\\)15 d, \\(2.47+0.12\\\-0.11\\) R\\(_\\)) that was first detected in the TESS photometry. Using follow-up observations with CHEOPS and HARPS, we refine the planetary radius of both planets, derive the mass of planet b (\\(4.5+1.5\\\-1.4\\) M\\(_\\)) and confirm the planetary nature of planet c. Intriguingly, a third periodic signal is clearly detected in our HARPS RVs that we cannot link to stellar activity. This signal could be attributed to a third planet (P\\(\\)38 d, Msin(i)=\\(26.4+6.3\\\-6.8\\) M\\(_\\)) in the system, however with the current photometric dataset we do not find a transit. Our dynamical analysis highlights that this potential outer planet would remain stable. Using the precise radius and mass for TOI-4311 b we model its interior structure and find that it is very dense given the host star's galactic kinematics and chemistry. Hence this system could challenge current formation theories and provide insights into planet formation across the galaxy.

• Publisher: Cornell University Library, arXiv.org
• Subject: Extrasolar planets / Photometry / Planet formation / Planetary systems / Stellar activity / Stellar kinematics