Evidence for a volcanic atmosphere on the sub-Earth L98-59b
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| Format: | Preprint |
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2025
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| author | Bello-Arufe, Aaron Damiano, Mario Bennett, Katherine A. Hu, Renyu Welbanks, Luis MacDonald, Ryan J. Seligman, Darryl Z. Sing, David K. Tokadjian, Armen Oza, Apurva Yang, Jeehyun |
| author_facet | Bello-Arufe, Aaron Damiano, Mario Bennett, Katherine A. Hu, Renyu Welbanks, Luis MacDonald, Ryan J. Seligman, Darryl Z. Sing, David K. Tokadjian, Armen Oza, Apurva Yang, Jeehyun |
| contents | Assessing the prevalence of atmospheres on rocky planets around M-dwarf stars is a top priority of exoplanet science. High-energy activity from M-dwarfs can destroy the atmospheres of these planets, which could explain the lack of atmosphere detections to date. Volcanic outgassing has been proposed as a mechanism to replenish the atmospheres of tidally-heated rocky planets. L 98-59 b, a sub-Earth transiting a nearby M dwarf, was recently identified as the most promising exoplanet to detect a volcanic atmosphere. We present the transmission spectrum of L 98-59 b from four transits observed with JWST NIRSpec G395H. Although the airless model provides an adequate fit to the data based on its $χ^2$, an SO$_2$ atmosphere is preferred by 3.6$σ$ over a flat line in terms of the Bayesian evidence. Such an atmosphere would likely be in a steady state where volcanism balances escape. If so, L 98-59 b must experience at least eight times as much volcanism and tidal heating per unit mass as Io. If volcanism is driven by runaway melting of the mantle, we predict the existence of a subsurface magma ocean in L 98-59 b extending up to $R_p\sim 60-90\%$. An SO$_2$-rich volcanic atmosphere on L 98-59 b would be indicative of an oxidized mantle with an oxygen fugacity of $f\rm{O}_2>IW+2.7$, and it would imply that L 98-59 b must have retained some of its volatile endowment despite its proximity to its star. Our findings suggest that volcanism may revive secondary atmospheres on tidally heated rocky planets around M-dwarfs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2501_18680 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Evidence for a volcanic atmosphere on the sub-Earth L98-59b Bello-Arufe, Aaron Damiano, Mario Bennett, Katherine A. Hu, Renyu Welbanks, Luis MacDonald, Ryan J. Seligman, Darryl Z. Sing, David K. Tokadjian, Armen Oza, Apurva Yang, Jeehyun Earth and Planetary Astrophysics Assessing the prevalence of atmospheres on rocky planets around M-dwarf stars is a top priority of exoplanet science. High-energy activity from M-dwarfs can destroy the atmospheres of these planets, which could explain the lack of atmosphere detections to date. Volcanic outgassing has been proposed as a mechanism to replenish the atmospheres of tidally-heated rocky planets. L 98-59 b, a sub-Earth transiting a nearby M dwarf, was recently identified as the most promising exoplanet to detect a volcanic atmosphere. We present the transmission spectrum of L 98-59 b from four transits observed with JWST NIRSpec G395H. Although the airless model provides an adequate fit to the data based on its $χ^2$, an SO$_2$ atmosphere is preferred by 3.6$σ$ over a flat line in terms of the Bayesian evidence. Such an atmosphere would likely be in a steady state where volcanism balances escape. If so, L 98-59 b must experience at least eight times as much volcanism and tidal heating per unit mass as Io. If volcanism is driven by runaway melting of the mantle, we predict the existence of a subsurface magma ocean in L 98-59 b extending up to $R_p\sim 60-90\%$. An SO$_2$-rich volcanic atmosphere on L 98-59 b would be indicative of an oxidized mantle with an oxygen fugacity of $f\rm{O}_2>IW+2.7$, and it would imply that L 98-59 b must have retained some of its volatile endowment despite its proximity to its star. Our findings suggest that volcanism may revive secondary atmospheres on tidally heated rocky planets around M-dwarfs. |
| title | Evidence for a volcanic atmosphere on the sub-Earth L98-59b |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2501.18680 |