{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/toi-5005-b-a-super-neptune-in-the-savanna","title":"TOI-5005 b: A super-Neptune in the savanna near the ridge","arxiv_id":"2409.18129","date":"2024-09-26","proceeding":null,"authors":["A. Castro-González","J. Lillo-Box","D. J. Armstrong","L. Acuña","A. Aguichine","V. Bourrier","S. Gandhi","S. G. Sousa","E. Delgado-Mena","A. Moya","V. Adibekyan","A. C. M. Correia","D. Barrado","M. Damasso","J. N. Winn","N. C. Santos","K. Barkaoui","S. C. C. Barros","Z. Benkhaldoun","F. Bouchy","C. Briceño","D. A. Caldwell","K. A. Collins","Z. Essack","M. Ghachoui","M. Gillon","R. Hounsell","E. Jehin","J. M. Jenkins","M. A. F. Keniger","N. Law","A. W. Mann","L. D. Nielsen","F. J. Pozuelos","N. Schanche","S. Seager","T. -G. Tan","M. Timmermans","J. Villaseñor","C. N. Watkins","C. Ziegler"],"abstract":"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 $\\rho_{\\rm p}$ = $0.74 \\pm 0.16$ $\\rm g \\, cm^{-3}$. 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.","url_abs":"https://arxiv.org/abs/2409.18129v2","url_pdf":"https://arxiv.org/pdf/2409.18129v2.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"toi-5005-b-a-super-neptune-in-the-savanna","repo_url":"https://github.com/castro-gzlz/TESS-cont","is_official":1,"mentioned_in_paper":0,"mentioned_in_github":0,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}