Some ideas concerning the problem of anomalous polar E region heating due to Farley-Buneman turbulence

The energetics of the excitation of the Farley-Buneman instability is considered, which is recently observed in the auroral and equatorial E regions of the Earth's ionosphere at altitudes between 100 km and 120 km. In the magnetic field of the Earth the Farley-Buneman instability is excited under the condition of a strong enough external electric field in the case of ion-neutral collisions with frequencies much larger than the ion gyrofrequency and electron-neutral collisions with frequencies much below the electron gyrofrequency. It is shown that the linear increase of the wave amplitudes is caused by a small disbalance between the processes of nonlinear energy pumping into the wave from an external electric field and the energy loss because of the collisions of the electrons and ions with the neutral particles. During the nonlinear energy pumping energy of the external electric field is transferred into a nonlinear current of second order, which is connected with the oscillating motion of the electrons in the wave. The oscillating electron motion takes place perpendicular to wave propagation. From the estimations follows that the energy pumped into a Farley-Buneman wave during one period of pulsation is much larger than the wave energy itself. A new and simply to understand derivation of the anomalous diffusion coefficient is presented, related to the study of the behaviour of a test wave with frequency much above the frequencies of the Farley-Buneman turbulence in developed stage can cause an additional macroscopic nonlinear Pedersen current directed along the external electric field. It is found that the nonlinear Pedersen current can reach the order of the usual Pedersen current and should contribute to the effective heating of the ionospheric plasma.     

初始外围尺度与加热对台风次眼墙形成的影响北大核心

台风次眼墙位于主眼墙外侧,由次对流环和低层切向风次极大值两个基本结构组成。本文通过一系列理想数值试验讨论了不同初始涡旋外围风场结构对次眼墙形成的影响作用以及关键动力学过程。结果表明,次眼墙形成的时间和位置与初始涡旋外围尺度显著相关:随着外围尺度递减,台风从形成完整双眼墙、伪双眼墙到没有双眼墙逐步过渡,次眼墙形成时间推迟且位置更加靠近台风中心。动力学分析发现,初始外围尺度可控制外雨带分布,雨带的非绝热加热主导了主眼墙外围边界层径向入流和绝对涡度径向输送的分布和大小。绝对涡度径向输送和摩擦耗散的相对大小及位置决定了次眼墙低层切向风次极大值出现的可能性和位置。动量强迫对低层切向风次极大值的大小仍有贡献。     

台风“摩羯”和“利奇马”经渤海强度变化特征分析

利用FY 4水汽云图、NCEP/FNL资料、自动站资料和ERA Interim海温资料，分析入海增强台风“摩羯”（1814）和入海减弱台风“利奇马”（1909）经过渤海强度变化特征。结论如下：台风“摩羯”中心入海增强过程伴随着中高层冷空气侵入，冷空气深入“摩羯”云系中心，台风强度减弱并逐渐消亡。台风“利奇马”入海前冷空气已经侵入台风中心，台风入海后强度减弱,暖心结构变得不对称，低层有清晰的斜压特征。“摩羯”入海前渤海上空为强辐散区，“利奇马”入海前渤海上空为弱辐合场，北上前进方向出现高空辐散有利于台风加强。台风登陆前垂直风切变与台风强度反位相分布，北上后台风垂直风切变与台风强度同位相分布。“摩羯”入海后水汽通道出现断裂，其入海增强更多依赖于热力条件和动力条件。“利奇马”水汽通量和水汽通量散度源于自身环流的贡献。台风“摩羯”入海后潜热加热率激增，“利奇马”低层维持弱潜热加热直至台风消亡。     

蒸汽冷凝过程的分子团聚模型及其对不凝性气体影响传热性能的解释

根据相变过程的微观物理机理和热力学特性,提出了冷凝传热过程中,近壁面蒸汽分子经由团聚阶段进而冷凝成宏观液滴的物理模型.并将团聚体分布与滴状冷凝传热性能相联系,从而研究不凝性气体对滴状冷凝传热过程的影响.在改进的Dillmann和Meier(DM)模型基础上,将分子团聚过程中的临界过饱和度与冷凝过程中的过冷度相联系,以及将团聚体的能量特性与液固界面物理化学特性相联系,将团聚模型与考虑固液界面效应的滴状冷凝传热模型相联系,建立了近壁面条件影响的分子团聚模型.利用模型计算了近壁面蒸汽中团簇体尺寸和分布,以及不凝