Mass determination of the three long-period Neptune- and sub-Neptune-sized planets transiting TOI-282
Fuente:
arXiv
Salvato in:
| Autori principali: | , , , , , , , , , , , , , , , , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2025
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866914142491770880 |
|---|---|
| author | Barone, A. Rodler, F. Gandolfi, D. Bonfanti, A. Leonardi, P. Visca, L. Fridlund, M. Brogi, M. Fossati, L. Cubillos, P. E. Cochran, W. D. Csizmadia, S. Livingston, J. Nowak, G. Pallé, E. Persson, C. M. Redfield, S. Schmerling, H. Smith, A. M. S. |
| author_facet | Barone, A. Rodler, F. Gandolfi, D. Bonfanti, A. Leonardi, P. Visca, L. Fridlund, M. Brogi, M. Fossati, L. Cubillos, P. E. Cochran, W. D. Csizmadia, S. Livingston, J. Nowak, G. Pallé, E. Persson, C. M. Redfield, S. Schmerling, H. Smith, A. M. S. |
| contents | TOI-282 is a bright (V=9.38) F8 main-sequence star known to host three transiting long-period ($P_b$=22.9 d, $P_c$=56.0 d, and $P_d$=84.3 d) small ($R_p\approx$ 2-4 $R_{\oplus}$) planets. The orbital period ratio of the two outermost planets, namely TOI-282 c and d, is close to the 3:2 commensurability, suggesting that the planets might be trapped in a mean motion resonance. We combined space-borne photometry from the TESS telescope with high-precision HARPS and ESPRESSO Doppler measurements to refine orbital parameters, measure the planetary masses, and investigate the architecture and evolution of the system. We performed a Markov chain Monte Carlo joint analysis of the transit light curves and radial velocity time series, and carried out a dynamical analysis to model transit timing variations and Doppler measurements along with N-body integration. In agreement with previous results, we found that TOI-282 b, c, and d have radii of $R_b=2.69 \pm 0.23 \ R_{\oplus}$, $R_c=4.13^{+0.16}_{-0.14} \ R_{\oplus}$, and $R_d=3.11 \pm 0.15 \ R_{\oplus}$, respectively. We measured planetary masses of $M_b=6.2\pm1.6 \ M_{\oplus}$, $M_c=9.2\pm2.0 \ M_{\oplus}$, and $M_d=5.8^{+0.9}_{-1.1} \ M_{\oplus}$, which imply mean densities of $ρ_b=1.8^{+0.7}_{-0.6} \ \text{g cm}^{-3}$, $ρ_c=0.7 \pm 0.2 \ \text{g cm}^{-3}$, and $ρ_d=1.1^{+0.3}_{-0.2} \ \text{g cm}^{-3}$, respectively. The three planets may be water worlds, making TOI-282 an interesting system for future atmospheric follow-up observations with JWST and ELT. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_05147 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Mass determination of the three long-period Neptune- and sub-Neptune-sized planets transiting TOI-282 Barone, A. Rodler, F. Gandolfi, D. Bonfanti, A. Leonardi, P. Visca, L. Fridlund, M. Brogi, M. Fossati, L. Cubillos, P. E. Cochran, W. D. Csizmadia, S. Livingston, J. Nowak, G. Pallé, E. Persson, C. M. Redfield, S. Schmerling, H. Smith, A. M. S. Earth and Planetary Astrophysics TOI-282 is a bright (V=9.38) F8 main-sequence star known to host three transiting long-period ($P_b$=22.9 d, $P_c$=56.0 d, and $P_d$=84.3 d) small ($R_p\approx$ 2-4 $R_{\oplus}$) planets. The orbital period ratio of the two outermost planets, namely TOI-282 c and d, is close to the 3:2 commensurability, suggesting that the planets might be trapped in a mean motion resonance. We combined space-borne photometry from the TESS telescope with high-precision HARPS and ESPRESSO Doppler measurements to refine orbital parameters, measure the planetary masses, and investigate the architecture and evolution of the system. We performed a Markov chain Monte Carlo joint analysis of the transit light curves and radial velocity time series, and carried out a dynamical analysis to model transit timing variations and Doppler measurements along with N-body integration. In agreement with previous results, we found that TOI-282 b, c, and d have radii of $R_b=2.69 \pm 0.23 \ R_{\oplus}$, $R_c=4.13^{+0.16}_{-0.14} \ R_{\oplus}$, and $R_d=3.11 \pm 0.15 \ R_{\oplus}$, respectively. We measured planetary masses of $M_b=6.2\pm1.6 \ M_{\oplus}$, $M_c=9.2\pm2.0 \ M_{\oplus}$, and $M_d=5.8^{+0.9}_{-1.1} \ M_{\oplus}$, which imply mean densities of $ρ_b=1.8^{+0.7}_{-0.6} \ \text{g cm}^{-3}$, $ρ_c=0.7 \pm 0.2 \ \text{g cm}^{-3}$, and $ρ_d=1.1^{+0.3}_{-0.2} \ \text{g cm}^{-3}$, respectively. The three planets may be water worlds, making TOI-282 an interesting system for future atmospheric follow-up observations with JWST and ELT. |
| title | Mass determination of the three long-period Neptune- and sub-Neptune-sized planets transiting TOI-282 |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2511.05147 |