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| Format: | Preprint |
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2025
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| Online-Zugang: | https://arxiv.org/abs/2511.13832 |
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| author | Alves, Douglas R. Jenkins, James S. Vinés, José I. Moyano, Maximilano Anderson, David R. Magliano, Christian Covone, Giovanni Stassun, Keivan G. Soubkiou, Abderahmane Gillen, Edward Battley, Matthew P. Hughes, Alexander Armstrong, David J. Saha, Suman Hawthorn, Faith Wheatley, Peter J. Collins, Karen A. Schwarz, Richard P. Srdoc, Gregor Apergis, Ioannis Zivave, Tafadzwa Lendl, Monika Tofflemire, Benjamin M. Doty, John P. Hedges, Christina Mireles, Ismael Burleigh, Matthew R. Kendall, Alicia Harvey, George T. Goad, Michael R. Casewell, Sarah L. Edkins, Troy |
| author_facet | Alves, Douglas R. Jenkins, James S. Vinés, José I. Moyano, Maximilano Anderson, David R. Magliano, Christian Covone, Giovanni Stassun, Keivan G. Soubkiou, Abderahmane Gillen, Edward Battley, Matthew P. Hughes, Alexander Armstrong, David J. Saha, Suman Hawthorn, Faith Wheatley, Peter J. Collins, Karen A. Schwarz, Richard P. Srdoc, Gregor Apergis, Ioannis Zivave, Tafadzwa Lendl, Monika Tofflemire, Benjamin M. Doty, John P. Hedges, Christina Mireles, Ismael Burleigh, Matthew R. Kendall, Alicia Harvey, George T. Goad, Michael R. Casewell, Sarah L. Edkins, Troy |
| contents | Observations have shown that planets similar to Neptune are rarely found orbiting Sun-like stars with periods up to ~4 days, defining the so-called Neptune desert region. Therefore, the detection of each individual planet in this region holds a high value, providing detailed insights into how such a population came to form and evolve. Here we report the detection of TOI-333b, a Neptune desert planet with a mass, radius, and bulk density of 20.1 $\pm$ 2.4 M$_{\oplus}$, 4.26 $\pm$ 0.11 R$_{\oplus}$, and 1.42 $\pm$ 0.21 \gccc, respectively. The planet orbits a F7V star every 3.78 d, whose mass, radius and effective temperature are of 1.2 $\pm$ 0.1 \msun, 1.10 $\pm$ 0.03 \rsun, and 6241$^{+73}_{-62}$ K, respectively. TOI-333b is likely younger than 1 Gyr, which is supported by the presence of the doublet Li line around 6707.856 textup{~Å} and its comparison to Li abundances in open clusters with well constrained ages. The planet is expected to host only 8.5$^{+10.9}_{-8.3}\%$ gas-to-core mass ratio for a H/He envelope. On the other hand, irradiated ocean world models predict 20$^{+11}_{-10}\%$ H$_2$O mass fraction with a core fraction of 35$^{+20}_{-23}\%$. Therefore, we expect that TOI-333b internal composition may be dominated by a pure rocky composition with almost no H/He envelope, or a rocky world with almost equal mass fraction of water. Finally, TOI-333b is more massive and larger than 77$\%$ and 82$\%$ of its Neptune desert counterparts, respectively, while its host ranks among the hottest known for Neptune Desert planets, making this system a unique laboratory to study the evolution of such planets around hot stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_13832 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | TOI-333b: A Neptune Desert planet around a F7V star Alves, Douglas R. Jenkins, James S. Vinés, José I. Moyano, Maximilano Anderson, David R. Magliano, Christian Covone, Giovanni Stassun, Keivan G. Soubkiou, Abderahmane Gillen, Edward Battley, Matthew P. Hughes, Alexander Armstrong, David J. Saha, Suman Hawthorn, Faith Wheatley, Peter J. Collins, Karen A. Schwarz, Richard P. Srdoc, Gregor Apergis, Ioannis Zivave, Tafadzwa Lendl, Monika Tofflemire, Benjamin M. Doty, John P. Hedges, Christina Mireles, Ismael Burleigh, Matthew R. Kendall, Alicia Harvey, George T. Goad, Michael R. Casewell, Sarah L. Edkins, Troy Earth and Planetary Astrophysics Solar and Stellar Astrophysics Observations have shown that planets similar to Neptune are rarely found orbiting Sun-like stars with periods up to ~4 days, defining the so-called Neptune desert region. Therefore, the detection of each individual planet in this region holds a high value, providing detailed insights into how such a population came to form and evolve. Here we report the detection of TOI-333b, a Neptune desert planet with a mass, radius, and bulk density of 20.1 $\pm$ 2.4 M$_{\oplus}$, 4.26 $\pm$ 0.11 R$_{\oplus}$, and 1.42 $\pm$ 0.21 \gccc, respectively. The planet orbits a F7V star every 3.78 d, whose mass, radius and effective temperature are of 1.2 $\pm$ 0.1 \msun, 1.10 $\pm$ 0.03 \rsun, and 6241$^{+73}_{-62}$ K, respectively. TOI-333b is likely younger than 1 Gyr, which is supported by the presence of the doublet Li line around 6707.856 textup{~Å} and its comparison to Li abundances in open clusters with well constrained ages. The planet is expected to host only 8.5$^{+10.9}_{-8.3}\%$ gas-to-core mass ratio for a H/He envelope. On the other hand, irradiated ocean world models predict 20$^{+11}_{-10}\%$ H$_2$O mass fraction with a core fraction of 35$^{+20}_{-23}\%$. Therefore, we expect that TOI-333b internal composition may be dominated by a pure rocky composition with almost no H/He envelope, or a rocky world with almost equal mass fraction of water. Finally, TOI-333b is more massive and larger than 77$\%$ and 82$\%$ of its Neptune desert counterparts, respectively, while its host ranks among the hottest known for Neptune Desert planets, making this system a unique laboratory to study the evolution of such planets around hot stars. |
| title | TOI-333b: A Neptune Desert planet around a F7V star |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2511.13832 |