发表机构
Institute of Science and Technology for Deep Space Exploration, Nanjing University; School of Physics and Astronomy, Sun Yat-Sen University; CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area; State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology; Atmospheric, Oceanic, and Planetary Physics Department, University of Oxford; Department of Physics and Astronomy, University of Exeter; Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University（南京大学深空探测科学与技术研究院; 中山大学物理学院; 粤港澳大湾区空间望远镜科学中心; 澳门科技大学月与行星科学国家重点实验室; 牛津大学大气、海洋与行星物理系; 埃克塞特大学物理与天文系; 上海交通大学李政道研究所及物理与天文学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究量化了垂直混合能量输运对蓬松金星大气-内部耦合的影响，发现其提供类温室加热、改变热结构与挥发物分配，并重塑中红外光谱，影响半径估计。
AI 中文摘要
高度辐照、低密度的岩石行星，如“蓬松金星”，可能在其大气与岩浆洋内部之间存在强耦合。以往研究主要通过辐射传输和化学平衡处理这种耦合，而垂直混合的作用尚不明确。本文量化了与垂直混合相关的能量输运如何改变蓬松金星的热结构、挥发性化学和发射光谱。大气环流和重力波破碎是这种输运可能的动力学来源。我们表明，这种能量输运通过加热深层大气提供了一种额外的类温室加热路径，从而增加了岩浆洋表面的压力和温度。由此产生的热变化也重塑了大气成分，尤其是CO和H2O的丰度，并改变了含C、H、O的挥发性物质在大气与岩浆洋之间的分配。此外，这些变化重塑了中红外行星-恒星通量比，尤其是在低平衡温度和较高质量行星中。在高C/O下，它略微增加了3.5–4.0微米附近的通量，但更广泛地降低了大气透明度并抑制了通量。这可能在有限温度范围内影响蓬松金星半径的估计。
英文摘要
Highly irradiated, underdense rocky planets such as puffy Venuses may host strong coupling between their atmospheres and magma-ocean interiors. Previous studies have mainly treated this coupling through radiative transfer and chemical equilibrium, leaving the role of vertical mixing unclear. Here we quantify how energy transport associated with vertical mixing modifies the thermal structure, volatile chemistry, and emission spectra of puffy Venuses. Atmospheric circulation and gravity-wave breaking are possible dynamical sources of such transport. We show that this energy transport provides an additional greenhouse-like heating pathway by warming the deep atmosphere, thereby increasing the pressure and temperature at the magma-ocean surface. The resulting thermal changes also reshape the atmospheric composition, especially the abundances of \ce{CO} and \ce{H2O}, and change the partitioning of C-, H-, and O-bearing volatiles between the atmosphere and the magma ocean. Moreover, these changes reshape the mid-infrared planet--star flux ratio, especially at low equilibrium temperatures and in higher-mass planets. Under high C/O, it slightly increases the flux near $3.5$--$4.0\,μ$m, but more broadly reduces atmospheric transparency and suppresses the flux. This may affect radius estimates for puffy Venuses over a limited temperature range.
Comments24 pages, 13 figures. Accepted for publication in ApJ
