一次飑线风暴的环境条件和雷达回波特征分析

利用常规气象观测和新一代天气雷达监测资料,对大兴安岭地区加格达奇市2006年8月一次飑线天气的环境条件和雷达回波特征等分析发现：此次过程的影响系统高空槽为前倾结构,飑线发生在地面冷锋前,大气具有较强的不稳定层结,有利于上升运动,水汽充足,低层较强的垂直风切变使对流云团和弓形等线状回波生成并较长时间地维持和发展。对流云团位置与上升运动区域较为一致,产生飑线的强对流云团出现在中低层垂直速度梯度较大并靠近上升运动中心一侧,并位于低层比湿和水汽通量散度梯度较大区域即干锋附近以及K指数能量锋上。飑线弓形回波出现在一个中尺度椭圆状对流云团中心内部发展最强处。当云团向东北偏东方向移过加格达奇雷达站时,雷达反射率因子先后呈现出弓形、＂人＂字形等线状回波特征,当线状回波南端＂人＂字形顶部较强回波和后侧入流急流前方＂V＂型槽口的尖峰移经加格达奇时,带来了雷雨大风天气。     

2017年秋季河北一次飑线引发的雷暴大风过程分析

利用常规地面高空观测资料、地面自动站资料、NCEP 1°×1°再分析资料、卫星云图、多普勒天气雷达资料等,对2017年秋季发生在河北省中部的一次由飑线引发的雷暴大风天气进行分析。结果表明：本次雷暴大风过程发生在高空冷涡底部,槽后冷空气与低层暖平流叠加配合地面冷锋的有利天气背景下,由飑线回波直接造成。环境条件中水汽和热力达到了中国华北地区产生强雷暴大风的平均值,大气温度直减率和垂直风切变比夏季更适宜,但能量不如夏季充足。飑线的强度、形态与夏季产生雷暴大风的雷达回波特征无异,但依据低层径向速度大值区预警秋季飑线大风需提高阈值。秋季飑线过程中地面同样伴随风场辐合、雷暴高压等中尺度系统,冷池密度流作用有利于地面大风产生。     

台风“麦莎”的强度对台风前部飑线发展过程影响的研究

对2005年8月5日16时(UTC,下同)至6日00时发生的一次台风前部飑线过程进行了数值模拟,分析表明:台前飑线在母体台风和副高之间的湿区生成。台风为这次台前飑线过程提供了有利的条件,包括强的低空急流输送充沛的水汽,强的不稳定环境产生大的对流有效位能以及强的地表辐合,使得初始的离散的对流单体组织发展形成台前飑线。成熟时期的台前飑线虽然比中纬度和热带飑线的变压强度小,但是具有更强的低层暖湿空气入流,中层的入流范围也更加宽广。敏感性试验结果表明:台风强度越强,其台前飑线的回波强度越强,移动速度更快,生命史也更长。强台风使得低空垂直风切变更大,有利于台前飑线的生成和发展,在台前飑线发展成熟后,低空垂直风切变强度减小,不利于台前飑线的维持,加之低空水汽输送的减少,使其逐渐趋向衰亡。     

飑线的研究进展

飑线是一种线状的中尺度对流系统,发生时破坏力大,可以产生严重的经济损失和人员伤亡。在我国,几乎每年都会出现由飑线引起的巨大损失。近年来,国内外对飑线的研究不断发展,无论是从大尺度环流背景、形成机制、组织形式、内部结构还是维持机制都有了较为深入的研究。深入研究飑线的形成过程,对于预报和灾害预警、防护,都具有很重要的意义。     

Combining optical spectroscopy and interferometry

Modern optical spectrographs and optical interferometers push the limits in the spectral and spatial regime, providing important new tools for the exploration of the Universe. In this contribution I outline the complementary nature of spectroscopic and interferometric observations and discuss different strategies for combining such data. Most remarkable, the latest generation of “spectro‐interferometric” instruments combine the milliarcsecond angular resolution achievable with interferometry with spectral capabilities, enabling direct constraints on the distribution, density, kinematics, and ionization structure of the gas component in protoplanetary disks. I will present some selected studies from the field of star‐ and planet formation and hot star research in order to illustrate these fundamentally new observational opportunities. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Studies of accretion flows around rotating black holes – I. Particle dynamics in a pseudo-Kerr potential

We study the formation of the absorption features, called the cyclotron–annihilation lines, in the γ-spectra of the neutron stars (pulsars), owing to the fundamental quantum-electrodynamic effect of the one–photon pair creation in magnetized vacuum. As a result, we substantiate a new method for the determination of the neutron star magnetic fields B based on measuring the interval between the main annihilation and the first cyclotron–annihilation absorption lines. It is found that these lines may be easily resolved, and, consequently, the method is surely applicable if the following conditions are satisfied. (i) A γ-source has to be compact enough and located near a star, but not close to its magnetic poles. For instance, it may be a disc in the plane of a star magnetic equator with latitudinal angular width less than     and radial extent up to 25 per cent of the star radius. (ii) The source is to produce detectable γ-radiation at large angles ≳60° to the local magnetic field. Being situated in a closed field line region and having a broad radiation pattern, such a source is not what is usually considered in the context of the polar cap and outer gap models of the pulsar γ-emission dealing with open field lines only. (iii) Magnetic field strength must lie in a certain narrow interval with the centre at  ∼(3–4) × 10¹²  G. Its width depends on the star orientation and disc radial extend and in the most favourable case is about 20–30 per cent of its lower boundary. Finally, the influence of the star rotation on this method employment is considered and new possibilities arising from forthcoming polarization observations are briefly discussed.     

关于高维代数族的nef-值态射的结构

设M是有末端奇点的n维正规代数簇，L是M上的丰富线丛,（M,L）的数字有效值为τ=u/v（u、v是互素的正整数），φ：M→X是由（M，L）决定的nef-值态射，F是φ的一般纤维。通过研究τ的取值情况对（M，L）进行分类．给出了当u=n＋1，n时（M,L）和（F，LF）的较完整的分类，推广了一些文献的结果。