Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet With a White Dwarf Companion
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2024
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| author | Saidel, Morgan Vissapragada, Shreyas Spake, Jessica Knutson, Heather A. Linssen, Dion Zhang, Michael Greklek-McKeon, Michael González, Jorge Pérez Oklopčić, Antonija |
| author_facet | Saidel, Morgan Vissapragada, Shreyas Spake, Jessica Knutson, Heather A. Linssen, Dion Zhang, Michael Greklek-McKeon, Michael González, Jorge Pérez Oklopčić, Antonija |
| contents | The lack of close-in Neptune-mass exoplanets evident in transit surveys has largely been attributed either to photoevaporative mass loss or high-eccentricity migration. To distinguish between these two possibilities, we investigate the origins of TOI-1259 A b, a Saturn-mass (0.4 M$_J$, 1.0 R$_J$) exoplanet lying along the upper edge of the Neptune desert. TOI-1259 A b's close-in ($P$ = 3.48 days) orbit and low bulk density make the planet particularly vulnerable to photoevaporation. Using transits observed in the 1083 nm metastable helium line, we probe the upper atmosphere of TOI-1259 A b with the Hale Telescope at Palomar Observatory and the Near-Infrared Spectrograph on Keck II. We report an excess absorption of $0.395\pm{0.072}\%$ with Palomar and a blueshifted absorption of $2.4\pm0.52\%$ with Keck, consistent with an extended escaping atmosphere. Fitting this signal with a Parker wind model, we determine a corresponding atmospheric mass loss rate of log($\dot{M}$) = $10.33\pm 0.13$ g/s for a thermosphere temperature of $8400^{+1200}_{-1000}$ K based on the Palomar absorption and log($\dot{M}$) = $10.0\pm 0.1$ g/s for a thermosphere temperature of $8200^{+1000}_{-900}$ K based on the Keck absorption. This relatively low rate suggests that this planet would not have been significantly altered by mass loss even if it formed in-situ. However, the presence of a white dwarf companion, TOI-1259 B, hints that this planet may not have formed close-in, but rather migrated inward relatively late. Given the estimated parameters of the proto-white dwarf companion, we find that high-eccentricity migration is possible for the system. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_08736 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet With a White Dwarf Companion Saidel, Morgan Vissapragada, Shreyas Spake, Jessica Knutson, Heather A. Linssen, Dion Zhang, Michael Greklek-McKeon, Michael González, Jorge Pérez Oklopčić, Antonija Earth and Planetary Astrophysics Solar and Stellar Astrophysics The lack of close-in Neptune-mass exoplanets evident in transit surveys has largely been attributed either to photoevaporative mass loss or high-eccentricity migration. To distinguish between these two possibilities, we investigate the origins of TOI-1259 A b, a Saturn-mass (0.4 M$_J$, 1.0 R$_J$) exoplanet lying along the upper edge of the Neptune desert. TOI-1259 A b's close-in ($P$ = 3.48 days) orbit and low bulk density make the planet particularly vulnerable to photoevaporation. Using transits observed in the 1083 nm metastable helium line, we probe the upper atmosphere of TOI-1259 A b with the Hale Telescope at Palomar Observatory and the Near-Infrared Spectrograph on Keck II. We report an excess absorption of $0.395\pm{0.072}\%$ with Palomar and a blueshifted absorption of $2.4\pm0.52\%$ with Keck, consistent with an extended escaping atmosphere. Fitting this signal with a Parker wind model, we determine a corresponding atmospheric mass loss rate of log($\dot{M}$) = $10.33\pm 0.13$ g/s for a thermosphere temperature of $8400^{+1200}_{-1000}$ K based on the Palomar absorption and log($\dot{M}$) = $10.0\pm 0.1$ g/s for a thermosphere temperature of $8200^{+1000}_{-900}$ K based on the Keck absorption. This relatively low rate suggests that this planet would not have been significantly altered by mass loss even if it formed in-situ. However, the presence of a white dwarf companion, TOI-1259 B, hints that this planet may not have formed close-in, but rather migrated inward relatively late. Given the estimated parameters of the proto-white dwarf companion, we find that high-eccentricity migration is possible for the system. |
| title | Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet With a White Dwarf Companion |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2404.08736 |