Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b

J. M. Almenara, X. Bonfils, T. Guillot, M. Timmermans, R. F. Díaz, J. Venturini, A. C. Petit, T. Forveille, O. Suárez, D. Mékarnia, A. H.M.J. Triaud, L. Abe, P. Bendjoya, F. Bouchy, J. Bouvier, L. Delrez, G. Dransfield, E. Ducrot, M. Gillon, M. J. HootonE. Jehin, A. W. Mann, R. Mardling, F. Murgas, A. Leleu, M. Lendl, D. Queloz, S. Seager, J. Winn, S. Zuñiga Fernández

Research output: Contribution to journalArticlepeer-review

1 Scopus citations


TOI-1227 b is an 11 Myr old validated transiting planet in the middle of its contraction phase, with a current radius of 0.85 RJ. It orbits a low-mass pre-main sequence star (0.170 M, 0.56 R) every 27.4 days. The magnetic activity of its young host star induces radial velocity jitter and prevents good measurements of the planetary mass. We gathered additional transit observations of TOI-1227 b with space- and ground-based telescopes, and we detected highly significant transit-timing variations (TTVs). Their amplitude is about 40 min and their dominant timescale is longer than 3.7 yr. Their most probable origin is dynamical interactions with additional planets in the system. We modeled the TTVs with inner and outer perturbers near first and second order resonances; several orbital configurations provide an acceptable fit. More data are needed to determine the actual orbital configuration and eventually measure the planetary masses. These TTVs and an updated transit chromaticity analysis reinforce the evidence that TOI-1227 b is a planet.

Original languageEnglish (US)
Article numberA96
JournalAstronomy and Astrophysics
StatePublished - Mar 1 2024

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


  • planetary systems
  • stars: individual: TOI-1227
  • stars: low-mass
  • stars: pre-main sequence
  • techniques: photometric


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