A very eccentric brown dwarf coplanar to a warm Jupiter and a hot super Earth
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| author | Jones, Matías I. Naponiello, Luca Trifonov, Trifon Brahm, Rafael Pichierri, Gabriele Acuña-Aguirre, Lorena De Rosa, Robert J. Pinto, Marcelo Tala Bonomo, Aldo S. Mancini, Luigi Sozzetti, Alessandro Reinarz, Yared Morbidelli, Alessandro Espinoza, Néstor Rosotti, Giovanni Nielsen, Eric L. Stefanov, Stefan Y. Henning, Thomas Jordán, Andrés Eberhardt, Jan Hatzes, Artie Vanzi, Leonardo Janik, Jan Kabath, Petr |
| author_facet | Jones, Matías I. Naponiello, Luca Trifonov, Trifon Brahm, Rafael Pichierri, Gabriele Acuña-Aguirre, Lorena De Rosa, Robert J. Pinto, Marcelo Tala Bonomo, Aldo S. Mancini, Luigi Sozzetti, Alessandro Reinarz, Yared Morbidelli, Alessandro Espinoza, Néstor Rosotti, Giovanni Nielsen, Eric L. Stefanov, Stefan Y. Henning, Thomas Jordán, Andrés Eberhardt, Jan Hatzes, Artie Vanzi, Leonardo Janik, Jan Kabath, Petr |
| contents | In transiting planetary systems, where planetary sizes are accurately determined from transit observations, the presence of transit timing variations (TTVs), especially when combined with radial velocity (RV) data, provides powerful constraints on masses and orbital eccentricities. Together, these measurements offer crucial insights into system architecture, formation mechanisms, and dynamical evolution. We present long-term RV and transit/TTV monitoring of the active and young star (age $\sim$1 Gyr) TOI-201, revealing an exceptional multi-planet system composed of a hot super-Earth (SE) transiting every 5.8 days, a warm Jupiter (WJ) on a 53-day orbit, and an eccentric (e = 0.622) low-mass brown dwarf (BD) on an approximately 8-year orbit, with an estimated mass of M$_{\rm BD}$ $\sim$ 16 Jupiter masses. The BD is the longest-period transiting object ever characterized via RVs, and the only one known to be coplanar with inner planets. The architecture of this system suggests that the SE was formed isolated and in the innermost region of the gaseous disc. On the other hand, the orbital configuration of the outer companions suggests a nearly in-situ formation of both objects, with the WJ forming in a dense inner disc. Alternatively, the BD might have formed farther out and migrated inward, while inflating its eccentricity due to interactions with the disc. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2604_23926 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | A very eccentric brown dwarf coplanar to a warm Jupiter and a hot super Earth Jones, Matías I. Naponiello, Luca Trifonov, Trifon Brahm, Rafael Pichierri, Gabriele Acuña-Aguirre, Lorena De Rosa, Robert J. Pinto, Marcelo Tala Bonomo, Aldo S. Mancini, Luigi Sozzetti, Alessandro Reinarz, Yared Morbidelli, Alessandro Espinoza, Néstor Rosotti, Giovanni Nielsen, Eric L. Stefanov, Stefan Y. Henning, Thomas Jordán, Andrés Eberhardt, Jan Hatzes, Artie Vanzi, Leonardo Janik, Jan Kabath, Petr Earth and Planetary Astrophysics Solar and Stellar Astrophysics In transiting planetary systems, where planetary sizes are accurately determined from transit observations, the presence of transit timing variations (TTVs), especially when combined with radial velocity (RV) data, provides powerful constraints on masses and orbital eccentricities. Together, these measurements offer crucial insights into system architecture, formation mechanisms, and dynamical evolution. We present long-term RV and transit/TTV monitoring of the active and young star (age $\sim$1 Gyr) TOI-201, revealing an exceptional multi-planet system composed of a hot super-Earth (SE) transiting every 5.8 days, a warm Jupiter (WJ) on a 53-day orbit, and an eccentric (e = 0.622) low-mass brown dwarf (BD) on an approximately 8-year orbit, with an estimated mass of M$_{\rm BD}$ $\sim$ 16 Jupiter masses. The BD is the longest-period transiting object ever characterized via RVs, and the only one known to be coplanar with inner planets. The architecture of this system suggests that the SE was formed isolated and in the innermost region of the gaseous disc. On the other hand, the orbital configuration of the outer companions suggests a nearly in-situ formation of both objects, with the WJ forming in a dense inner disc. Alternatively, the BD might have formed farther out and migrated inward, while inflating its eccentricity due to interactions with the disc. |
| title | A very eccentric brown dwarf coplanar to a warm Jupiter and a hot super Earth |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2604.23926 |