Paper

An Ultra-Short Period Super-Earth and Sub-Neptune Spanning the Radius Valley Orbiting the Kinematic Thick Disk Star TOI-2345

Smith, Alexis M S, Buder, Maximilian, Rauer, Heike, 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, Ratti, Francesco, Hasiba, Johann, 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, Vivien, Hugo G, Kiss, Laszlo L, Ulmer-Moll, Solène, Barros, Susana C C, Bárczy, Tamas, Bonfanti, Andrea, Egger, Jo Ann, Demangeon, Olivier D S, Deline, Adrien, Gandolfi, Davide, Keller, Tatiana, Stalport, Manu, Ehrenreich, David, Goeke, Robert, Csizmadia, Szilard, Correia, Alexandre C M, Pollacco, Don, Olofsson, Göran, Davies, Melvyn B, Ribas, Ignasi, Piazza, Daniele, Caldwell, Douglas A, Mordasini, Christoph, Jenkins, Jon M, Günther, Maximilian N, Gisbert, Peter, Fossati, Luca, Broeg, Christopher, Wolf, Sebastian, Andrew Col

2025

Overview

A crucial chemical link between stars and their orbiting exoplanets is thought to exist. If universal, this connection could affect the formation and evolution of all planets. Therefore, this potential vital link needs testing by characterising exoplanets around chemically-diverse stars. We present the discovery of two planets orbiting the metal-poor, kinematic thick-disk K-dwarf TOI-2345. TOI-2345 b is a super-Earth with a period of 1.05 days and TOI-2345 c is a sub-Neptune with a period of 21 days. In addition to the target being observed in 4 TESS sectors, we obtained 5 CHEOPS visits and 26 radial velocities from HARPS. By conducting a joint analysis of all the data, we find TOI-2345 b to have a radius of \\(1.504\\substack{+0.047\\\-0.044}\\) R\\(_\\oplus\\) and a mass of \\(3.49\\pm0.85\\) M\\(_\\oplus\\); and TOI-2345 c to have a radius of \\(2.451\\substack{+0.045\\\-0.046}\\) R\\(_\\oplus\\) and a mass of \\(7.27\\substack{+2.27\\\-2.45}\\) M\\(_\\oplus\\). To explore chemical links between these planets and their host star, we model their interior structures newly accounting for devolatised stellar abundances. TOI-2345 adds to the limited sample of well characterised planetary systems around thick disk stars. This system challenges theories of formation and populations of planets around thick disk stars with its Ultra-Short Period super-Earth and the wide period distribution of these two planets spanning the radius valley.

• Publisher: Cornell University Library, arXiv.org
• Subject: Extrasolar planets / Kinematics / Metallicity / Planetary orbits / Planetary systems / Stars