Bibcode
Heidari, N.; Alnajjarine, A.; Osborn, H. P.; Dragomir, D.; Dalba, P.; Benz, W.; Hébrard, G.; Laskar, J.; Billot, N.; Günther, M. N.; Wilson, T. G.; Alibert, Y.; Bonfanti, A.; Bieryla, A.; Broeg, C.; Correia, A. C. M.; Egger, J. A.; Essack, Z.; Furlan, E.; Gandolfi, D.; Grieves, N.; Howell, S.; LaCourse, D.; Pezzotti, C.; Pritchard, T.; Sousa, S. G.; Ulmer-Moll, S.; Villanueva, S.; Alonso, R.; Asquier, J.; Bárczy, T.; Barrado, D.; Barros, S. C. C.; Baumjohann, W.; Borsato, L.; Brandeker, A.; Buder, M.; Collier Cameron, A.; Csizmadia, S.; Cubillos, P. E.; Davies, M. B.; Deleuil, M.; Delfosse, X.; Deline, A.; Demangeon, O. D. S.; Demory, B.; Derekas, A.; Edwards, B.; Ehrenreich, D.; Erikson, A.; Fortier, A.; Fossati, L.; Fridlund, M.; Gazeas, K.; Gillon, M.; Güdel, M.; Hasiba, J.; Heitzmann, A.; Helling, C.; Jenkins, J. M.; Keller, T.; Kane, S. R.; Stassun, K. G.; Kiss, L. L.; Korth, J.; Lam, K. W. F.; Latham, D. W.; des Etangs, A. Lecavelier; Leleu, A.; Lendl, M.; Maxted, P. F. L.; McDermott, S.; Merín, B.; Mordasini, C.; Nascimbeni, V.; Nowak, G.; Olofsson, G.; Pagano, I.; Pallé, E.; Piotto, G.; Pollacco, D.; Queloz, D.; Ragazzoni, R.; Rauer, H.; Ribas, I.; Ricker, G.; Santos, N. C.; Scandariato, G.; Seager, S.; Ségransan, D.; Simon, A. E.; Smith, A. M. S.; Stalport, M.; Striegel, S.; Sulis, S.; Szabó, G. M.; Udry, S.; Van Grootel, V.; Vanderspek, R.; Venturini, J. et al.
Referencia bibliográfica
Astronomy and Astrophysics
Fecha de publicación:
3
2026
Revista
Número de citas
0
Número de citas referidas
0
Descripción
We present the characterisation of the TOI-6041 system, a bright (V = 9.84 ± 0.03) G7-type star hosting at least two planets. The inner planet, TOI-6041 b, is a warm Neptune with a radius of 4.55−0.17+0.18 R⊕, initially identified as a single-transit event in TESS photometry. Subsequent observations with TESS and CHEOPS revealed additional transits, enabling the determination of its 26.04945−0.00034+0.00033 orbital period and the detection of significant transit-timing variations (TTVs), exhibiting a peak-to-peak amplitude of about 1 hour. Radial-velocity (RV) measurements obtained with the APF spectrographs allowed us to place a 3σ upper mass limit of 28.9 M⊕ on TOI-6041 b. In addition, the RV data reveal a second companion, TOI-6041 c, on an 88 d orbit, with a minimum mass of 0.25 MJup. A preliminary TTV analysis suggested that the observed variations could be caused by gravitational perturbations from planet c; however, reproducing the observed amplitudes requires a relatively high eccentricity of about 0.3 for that planet. Our dynamical stability analysis indicates that such a configuration is dynamically viable and places a 1σ upper limit on the mass of TOI-6041 c at 0.8 MJup. An alternative is the presence of a third, low-mass planet located between planets b and c, or on an inner orbit relative to planet b ─ particularly near a mean-motion resonance with planet b ─ which could account for the observed variations. These findings remain tentative, and further RV and photometric observations are essential in to better constrain the mass of planet b and to refine the TTV modeling, thereby improving our understanding of the system's dynamical architecture.