TOI-5005 b: A super-Neptune in the savanna near the ridge
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| Format: | Preprint |
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2024
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| author | Castro-González, A. Lillo-Box, J. Armstrong, D. J. Acuña, L. Aguichine, A. Bourrier, V. Gandhi, S. Sousa, S. G. Delgado-Mena, E. Moya, A. Adibekyan, V. Correia, A. C. M. Barrado, D. Damasso, M. Winn, J. N. Santos, N. C. Barkaoui, K. Barros, S. C. C. Benkhaldoun, Z. Bouchy, F. Briceño, C. Caldwell, D. A. Collins, K. A. Essack, Z. Ghachoui, M. Gillon, M. Hounsell, R. Jehin, E. Jenkins, J. M. Keniger, M. A. F. Law, N. Mann, A. W. Nielsen, L. D. Pozuelos, F. J. Schanche, N. Seager, S. Tan, T. -G. Timmermans, M. Villaseñor, J. Watkins, C. N. Ziegler, C. |
| author_facet | Castro-González, A. Lillo-Box, J. Armstrong, D. J. Acuña, L. Aguichine, A. Bourrier, V. Gandhi, S. Sousa, S. G. Delgado-Mena, E. Moya, A. Adibekyan, V. Correia, A. C. M. Barrado, D. Damasso, M. Winn, J. N. Santos, N. C. Barkaoui, K. Barros, S. C. C. Benkhaldoun, Z. Bouchy, F. Briceño, C. Caldwell, D. A. Collins, K. A. Essack, Z. Ghachoui, M. Gillon, M. Hounsell, R. Jehin, E. Jenkins, J. M. Keniger, M. A. F. Law, N. Mann, A. W. Nielsen, L. D. Pozuelos, F. J. Schanche, N. Seager, S. Tan, T. -G. Timmermans, M. Villaseñor, J. Watkins, C. N. Ziegler, C. |
| contents | The Neptunian desert and savanna have recently been found to be separated by a ridge, an overdensity of planets in the period range of $\simeq$3-5 days. These features are thought to be shaped by dynamical and atmospheric processes, but their roles are not yet well understood. Our aim was to confirm and characterize the super-Neptune TESS candidate TOI-5005.01, which orbits a moderately bright (V = 11.8) solar-type star (G2 V) with an orbital period of 6.3 days. We confirm TOI-5005 b to be a transiting super-Neptune with a radius of $R_{\rm p}$ = $6.25\pm 0.24$ $\rm R_{\rm \oplus}$ ($R_{\rm p}$ = $0.558\pm 0.021$ $\rm R_{\rm J}$) and a mass of $M_{\rm p}$ = $32.7\pm 5.9$ $\rm M_{\oplus}$ ($M_{\rm p}$ = $0.103\pm 0.018$ $\rm M_{\rm J}$), which corresponds to a mean density of $ρ_{\rm p}$ = $0.74 \pm 0.16$ $\rm g \, cm^{-3}$. Our internal structure modelling indicates that the overall metal mass fraction is well constrained to a value slightly lower than that of Neptune and Uranus ($Z_{\rm planet}$ = $0.76^{+0.04}_{-0.11}$). We also estimated the present-day atmospheric mass-loss rate of TOI-5005 b, but found contrasting predictions depending on the choice of photoevaporation model. At a population level, we find statistical evidence ($p$-value = $0.0092^{+0.0184}_{-0.0066}$) that planets in the savanna such as TOI-5005 b tend to show lower densities than planets in the ridge, with a dividing line around 1 $\rm g \, cm^{-3}$, which supports the hypothesis of different evolutionary pathways populating the two regimes. TOI-5005 b is located in a key region of the period-radius space to study the transition between the Neptunian ridge and the savanna. It orbits the brightest star of all such planets, which makes it a target of interest for atmospheric and orbital architecture observations that will bring a clearer picture of its overall evolution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_18129 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | TOI-5005 b: A super-Neptune in the savanna near the ridge Castro-González, A. Lillo-Box, J. Armstrong, D. J. Acuña, L. Aguichine, A. Bourrier, V. Gandhi, S. Sousa, S. G. Delgado-Mena, E. Moya, A. Adibekyan, V. Correia, A. C. M. Barrado, D. Damasso, M. Winn, J. N. Santos, N. C. Barkaoui, K. Barros, S. C. C. Benkhaldoun, Z. Bouchy, F. Briceño, C. Caldwell, D. A. Collins, K. A. Essack, Z. Ghachoui, M. Gillon, M. Hounsell, R. Jehin, E. Jenkins, J. M. Keniger, M. A. F. Law, N. Mann, A. W. Nielsen, L. D. Pozuelos, F. J. Schanche, N. Seager, S. Tan, T. -G. Timmermans, M. Villaseñor, J. Watkins, C. N. Ziegler, C. Earth and Planetary Astrophysics The Neptunian desert and savanna have recently been found to be separated by a ridge, an overdensity of planets in the period range of $\simeq$3-5 days. These features are thought to be shaped by dynamical and atmospheric processes, but their roles are not yet well understood. Our aim was to confirm and characterize the super-Neptune TESS candidate TOI-5005.01, which orbits a moderately bright (V = 11.8) solar-type star (G2 V) with an orbital period of 6.3 days. We confirm TOI-5005 b to be a transiting super-Neptune with a radius of $R_{\rm p}$ = $6.25\pm 0.24$ $\rm R_{\rm \oplus}$ ($R_{\rm p}$ = $0.558\pm 0.021$ $\rm R_{\rm J}$) and a mass of $M_{\rm p}$ = $32.7\pm 5.9$ $\rm M_{\oplus}$ ($M_{\rm p}$ = $0.103\pm 0.018$ $\rm M_{\rm J}$), which corresponds to a mean density of $ρ_{\rm p}$ = $0.74 \pm 0.16$ $\rm g \, cm^{-3}$. Our internal structure modelling indicates that the overall metal mass fraction is well constrained to a value slightly lower than that of Neptune and Uranus ($Z_{\rm planet}$ = $0.76^{+0.04}_{-0.11}$). We also estimated the present-day atmospheric mass-loss rate of TOI-5005 b, but found contrasting predictions depending on the choice of photoevaporation model. At a population level, we find statistical evidence ($p$-value = $0.0092^{+0.0184}_{-0.0066}$) that planets in the savanna such as TOI-5005 b tend to show lower densities than planets in the ridge, with a dividing line around 1 $\rm g \, cm^{-3}$, which supports the hypothesis of different evolutionary pathways populating the two regimes. TOI-5005 b is located in a key region of the period-radius space to study the transition between the Neptunian ridge and the savanna. It orbits the brightest star of all such planets, which makes it a target of interest for atmospheric and orbital architecture observations that will bring a clearer picture of its overall evolution. |
| title | TOI-5005 b: A super-Neptune in the savanna near the ridge |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2409.18129 |