发表机构
University of Colorado Boulder; Laboratory for Atmospheric and Space Physics; University of Texas at Austin（科罗拉多大学博尔德分校; 大气与空间物理实验室; 德克萨斯大学奥斯汀分校）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过模拟极光电子束能谱对褐矮星大气的影响，检验极光加热能否解释JWST观测到的热反转，发现仅靠极光能量沉积无法同时匹配反转的幅度和压力水平，需考虑更强高能成分或其他加热机制。
AI 中文摘要
最近对Y型矮星CWISEPJ193518.59-154620.3（Faherty等人2024年；Suárez等人2025年）和T型矮星SIMPJ013656.5+093347.3（Nasedkin等人2025年）的JWST光谱建模表明，它们的大气中存在热反转，这意味着存在额外的加热源。极光能量沉积已被提出作为一种可能的机制。在这项工作中，我们对极光能量沉积过程及其产生的大气响应进行建模，以评估物理上合理的极光电子束能谱能否重现推断出的热反转。我们模拟了几种与木星极光电子群观测一致的极光电子束能谱的影响，并将其按褐矮星预期的总电子通量进行缩放。我们发现，仅靠极光能量沉积无法同时重现这两个天体推断出的反转幅度和压力水平。虽然我们的模型中产生了反转，但它们发生的压力水平相对于观测所需而言过低。这些结果表明，实际的极光电子群包含比本文考虑到的更强的高能成分，或者有其他加热机制对观测到的热反转有贡献，并且/或者大气的不均匀加热对于确定观测到的辐射很重要。
英文摘要
Recent modeling of the JWST spectra of the Y-dwarf CWISEPJ193518.59-154620.3 (Faherty et al. 2024; Suárez et al. 2025) and the T-dwarf SIMPJ013656.5+093347.3 (Nasedkin et al. 2025) indicates the presence of a thermal inversion in their atmospheres, implying an additional source of heating. Auroral energy deposition has been proposed as a potential mechanism. In this work, we model auroral energy deposition processes and the resulting atmospheric response to assess whether physically motivated auroral electron beam energy spectra can reproduce the inferred thermal inversions. We simulate the effects of several auroral electron beam energy spectra consistent with observations of the Jovian population of auroral electrons and scale them to the total electron flux expected for brown dwarfs. We find that auroral energy deposition alone cannot reproduce both the magnitude and pressure level of the inferred inversion in either object. While inversions are produced in our models, they occur at pressures that are too low compared to those required by the observations. These results suggest that the actual population of auroral electrons includes a stronger high-energy component than considered here, that additional heating mechanisms contribute to the observed thermal inversions, and/or that heterogeneous heating of the atmosphere is important for determining the observed emission.
