Simulations of Flare Chemistry in Brown Dwarf Companions to Active M Dwarfs
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arXiv
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866914027862491136 |
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| author | Gibbs, Aidan Fitzgerald, Michael P. |
| author_facet | Gibbs, Aidan Fitzgerald, Michael P. |
| contents | Brown dwarfs that are short period ($<10\,$day) companions to actively flaring M dwarfs may provide a context to directly observe flare-driven photochemistry and structural changes in an extrasolar planet-like atmosphere. To assess the viability of directly observing flare impacts in the atmosphere of a brown dwarf, we perform self-consistent temperature-chemistry modeling of the atmospheric response to individual energetic superflares. We modified the existing open-source \texttt{VULCAN} chemical-kinetics and \texttt{HELIOS} radiative-transfer codes for this purpose. Similar to previous studies of flare impacts on hydrogen dominated atmospheres, we find flares are capable of orders-of-magnitude changes in the mixing abundances of many chemical species, including important opacity sources like CH$_4$ and CO$_2$. However, due to fast chemical timescales resulting from high temperatures and densities in brown dwarf atmospheres, these changes last for a short-period of time, generally less than a day, and are only plausibly observable via high resolution emission spectroscopy. We find that the most observable, short-term spectral changes in hot (T$_{\text{eff}}\sim2000\,$K), high-gravity ($\log{\text{g}}\sim5$), cloudless brown dwarfs are the photolysis of H$_2$O and enhancement of CO$_2$, which can result in part-per-thousands spectral changes in the hours after a flare. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_07063 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Simulations of Flare Chemistry in Brown Dwarf Companions to Active M Dwarfs Gibbs, Aidan Fitzgerald, Michael P. Solar and Stellar Astrophysics Earth and Planetary Astrophysics Brown dwarfs that are short period ($<10\,$day) companions to actively flaring M dwarfs may provide a context to directly observe flare-driven photochemistry and structural changes in an extrasolar planet-like atmosphere. To assess the viability of directly observing flare impacts in the atmosphere of a brown dwarf, we perform self-consistent temperature-chemistry modeling of the atmospheric response to individual energetic superflares. We modified the existing open-source \texttt{VULCAN} chemical-kinetics and \texttt{HELIOS} radiative-transfer codes for this purpose. Similar to previous studies of flare impacts on hydrogen dominated atmospheres, we find flares are capable of orders-of-magnitude changes in the mixing abundances of many chemical species, including important opacity sources like CH$_4$ and CO$_2$. However, due to fast chemical timescales resulting from high temperatures and densities in brown dwarf atmospheres, these changes last for a short-period of time, generally less than a day, and are only plausibly observable via high resolution emission spectroscopy. We find that the most observable, short-term spectral changes in hot (T$_{\text{eff}}\sim2000\,$K), high-gravity ($\log{\text{g}}\sim5$), cloudless brown dwarfs are the photolysis of H$_2$O and enhancement of CO$_2$, which can result in part-per-thousands spectral changes in the hours after a flare. |
| title | Simulations of Flare Chemistry in Brown Dwarf Companions to Active M Dwarfs |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2509.07063 |