Structure and energy transfer of unstable hot star winds

Due to the instability of the radiation line force, the winds of hot, luminous stars should show a pronounced time-dependence resulting from the nonlinear growth of initially small perturbations. Following the method of Owocki, Castor & Rybicki (1988), we describe the time-dependent wind structure obtained with an independently developed code. Under the central assumption ofisothermality, our results are in very good agreement with the ones by Owocki et al. We find that the response of the wind to periodic base perturbations remains largely periodic, at least up tor 2...3R _* , with no clear evidence of stochastic behaviour.In order to test the foregoing assumption of isothermality and to compute the X-ray emission from models of structured winds, we have also incorporated theenergy equation into our simulations. We encountered the numerical problem that all radiative cooling zones collapse because of the oscillatory thermal instability (cf. Langer et al. 1981). We present a method to hinder this collapse by changing the cooling function at low temperatures. The resulting wind showsresolved cooling zones; but, for a supergiant wind relatively close to the star (r 10R _* ), the macroscopic wind structure is very similar to isothermal calculations. Most of the hot material is caused by shell-shell collisions.     

The sodium tail of the Moon

During the few days centered about new Moon, the lunar surface is optically hidden from Earth-based observers. However, the Moon still offers an observable: an extended sodium tail. The lunar sodium tail is the escaping “hot” component of a coma-like exosphere of sodium generated by photon-stimulated desorption, solar wind sputtering and meteoroid impact. Neutral sodium atoms escaping lunar gravity experience solar radiation pressure that drives them into the anti-solar direction forming a comet-like tail. During new Moon time, the geometry of the Sun, Moon and Earth is such that the anti-sunward sodium flux is perturbed by the terrestrial gravitational field resulting in its focusing into a dense core that extends beyond the Earth. An all-sky camera situated at the El Leoncito Observatory (CASLEO) in Argentina has been successfully imaging this tail through a sodium filter at each lunation since April 2006. This paper reports on the results of the brightness of the lunar sodium tail spanning 31 lunations between April 2006 and September 2008. Brightness variability trends are compared with both sporadic and shower meteor activity, solar wind proton energy flux and solar near ultra violet (NUV) patterns for possible correlations. Results suggest minimal variability in the brightness of the observed lunar sodium tail, generally uncorrelated with any single source, yet consistent with a multi-year period of minimal solar activity and non-intense meteoric fluxes.     

用单多卜勒雷达确定中尺度气旋环流中心及最大风速半径

首先给出具有 Ｒａｎｋｉｎｅ 模式的中尺度气旋的模拟多卜勒径向速度图,然后利用多卜勒雷达观测的径向速度与实际气流间的几何关系,提出一种确定近似轴对称的中尺度气旋中心及最大风速半径的方法。     

人居环境气候舒适度对城市创新的影响分析

以中国创新水平较高的91个地级及以上城市为研究对象,探讨人居环境气候舒适度对城市创新的影响程度。以城市发明专利申请数代表城市创新水平,采用温湿指数和风效指数的组合模型,参照相应的分级标准计算各城市年气候舒适期,分析城市人居环境气候舒适度与城市创新的关系。结果表明:气候舒适期每增加1%,发明专利申请数仅平均增加0.012%,相对于GDP、R&D人员全时当量、R&D经费等影响城市创新的关键因素,城市人居环境气候舒适度对城市创新有一定影响,但影响并不十分显著。因此,创新政策的着眼点在于关注城市创新投入、人力资本、经济规模等影响城市创新的关键因素。在此基础上,创新布局也应考虑人居环境气候舒适度因素。     

Multispacecraft Observations of Magnetic Clouds and Their Solar Origins between 19 and 23 May 2007

We analyze a series of complex interplanetary events and their solar origins that occurred between 19 and 23 May 2007 using observations by the STEREO and Wind satellites. The analyses demonstrate the new opportunities offered by the STEREO multispacecraft configuration for diagnosing the structure of in situ events and relating them to their solar sources. The investigated period was characterized by two high-speed solar wind streams and magnetic clouds observed in the vicinity of the sector boundary. The observing satellites were separated by a longitudinal distance comparable to the typical radial extent of magnetic clouds at 1 AU (fraction of an AU), and, indeed, clear differences were evident in the records from these spacecraft. Two partial-halo coronal mass ejections (CMEs) were launched from the same active region less than a day apart, the first on 19 May and the second on 20 May 2007. The clear signatures of the magnetic cloud associated with the first CME were observed by STEREO B and Wind while only STEREO A recorded clear signatures of the magnetic cloud associated with the latter CME. Both magnetic clouds appeared to have interacted strongly with the ambient solar wind and the data showed evidence that they were a part of the coronal streamer belt. Wind and STEREO B also recorded a shocklike disturbance propagating inside a magnetic cloud that compressed the field and plasma at the cloud’s trailing portion. The results illustrate how distant multisatellite observations can reveal the complex structure of the extension of the coronal streamer into interplanetary space even during the solar activity minimum. Electronic Supplementary Material  The online version of this article () contains supplementary material, which is available to authorized users.     

基于MISR多角度光学遥感影像的海面风速估算实验

太阳耀光是来自粗糙海面的直接太阳反射光,其强度与海面粗糙度密切相关,而海面粗糙度主要受海面风场影响。因此,包含太阳耀光信息的光学遥感影像在海洋动力过程和海面风速探测中具有积极意义。本文利用2016年2月到2017年3月期间成像的25幅Terra卫星MISR(Multi-angle Imaging Spectro Radiometer)传感器的多角度遥感影像,分别提取了太阳的高度角和方位角、正视和后视影像的卫星观测角、方位角等信息,校正获得正视和后视影像的太阳耀光辐射强度,进一步反演海表面粗糙度信息,进而计算海面风速。最后利用ECMWF(European Centre for Medium-Range Weather Forecasts)的模式风速数据与反演获得的风速结果进行对比验证。结果表明,两者的相关系数较高(R=0.745),均方根误差和平均绝对偏差值分别为1.514 m·s^-1和1.319 m·s^-1。初步实验结果表明,利用MISR多角度光学遥感影像估算海表面风速是可行性的。     

Kinematic features of a bow echo in southern China observed with doppler radar

A bow echo is a type of mesoscale convective phenomenon that often induces extreme weather and appears with strong reflectivity on radar images. A strong bow echo that developed from a supercell was observed over Foshan City in southern China on 17 April 2011. The intense gusty winds and showers caused huge losses of property and severely affected human lives. This paper presents an analysis of this strong meso- n-scale convective system based on Doppler radar observations. The isolated bow echo exhibited a horizontal scale of about 80 km in terms of reflectivity above 40 dBZ, and a life span of 8 hours. The system originated from the merging of a couple of weakly organized cells in a shear line, and developed into an arch shape as it moved through the shear zone. Sufficient surface moisture supply ensured the convective instability and development of the bow echo. The low-altitude winds retrieved from single Doppler radar observations showed an obvious rear-inflow jet along the notch area. Different from the conventional definition, no book- end anticyclone was observed throughout the life cycle. Very strong slantwise updrafts and downdrafts were recognizable from the retrieved winds, even though the spatial scale of the bow echo was small. Strong winds and induced damage on the surface are considered to have been caused by the mid-level rear-inflow jet and intense convective downdrafts.     

利用静止卫星云图进行二维傅里叶相位导风试验

根据二维傅里叶相位分析原理,对1 min间隔的IR云图进行由云推导风的反演。利用模块高度频数直方图把云分为高、中、低云。对连续三幅IR云图进行二维傅里叶相位导风计算,得到两个反演风场,对两个风场相同位置上的风矢进行逐点比较,剔除风向或风速差别较大的风矢,再对处理后的风场进行高度调整法的质量控制,把不合理的风矢剔除或调整到合理的高度层,得到连续性较好的风场。     

基于谱修正方法的非高斯风场模拟

为克服基于H erm ite谱修正方法的缺点,减少该方法中计算H erm ite多项式系数所需耗费的大量机时,提出了一种模拟非高斯风压场的新方法,采用非高斯累积分布函数（CDF）映射技术来代替基于H erm ite的概率密度函数（PDF）修正。选择任意边缘PDF模型作为概率目标模型,采用目标功率谱密度（PSD）作为样本函数,通过迭代修正该样本函数,使其收敛于目标概率密度函数和目标功率谱密度。将该方法应用于实际结构的非高斯风场模拟,模拟结果与目标谱符合良好,表明本文方法模拟非高斯风场具有较高的精确度和计算效率。     

冷空气引起的飞船主着陆场区偏北大风的特征分析及预报

分析了飞船主着陆场区1981—1999年1—4月和9—12月因冷空气而产生的偏北大风的过程中气候概况及其天气特征。通过分析发现:主着陆场区因冷空气引起的偏北大风以春季最频繁,秋、冬季最稀少;一天当中偏北大风以午后出现频率最大,午夜出现频率最少;对于不同季节的气压和温度,春、秋两季变化剧烈,冬季相对较小;在大风出现前24小时,主着陆场区的欧亚中高纬度大气环流以两槽一脊型、一槽一脊型、贝湖低压型为主;冷空气入侵前24小时,欧亚天气图上主着陆场区上游低层850hPa中高纬度有明显的冷中心,地面图场区上游冷高压中心的分布主要有3个区域:贝加尔湖西南至新疆、贝加尔湖到内蒙中北部、贝加尔湖西北部。大风前24小时在35～45°N、100～115°E等压线密集,等压线一般都在4根以上。