毛乌素沙漠边缘地区春末夏初沙尘暴天气的物理量场结构

沙尘暴天气是毛乌素沙漠边缘内蒙古、甘肃、宁夏、陕西等地区春末夏初特有的一种灾害性天气。应用欧洲中心再分析资料的气压场和各种物理量场,选取了5个沙尘暴个例,分析了沙尘暴时期各层气压场的特征和物理量的空间结构。结果表明：蒙古高压是影响沙尘暴的主要天气系统。在沙尘暴发生时,蒙古高压前部整层都为宽广而强劲的西北气流,从地面可伸展到200 hPa附近,其物理属性是干、冷,其前部近乎于东北—西南向的区域,是锋区的密集带,也是各种物理量表现最为敏感的区域,垂直速度场为上升运动区,涡度场为正涡度区,高—低层散度差值场为正值,这些物理量都为沙尘暴的发生起到了推动和加强作用。     

Toroidal versus poloidal magnetic fields in Sun-like stars: a rotation threshold

From a set of stellar spectropolarimetric observations, we report the detection of surface magnetic fields in a sample of four solar-type stars, namely HD 73350, HD 76151, HD 146233 (18 Sco) and HD 190771. Assuming that the observed variability of polarimetric signal is controlled by stellar rotation, we establish the rotation periods of our targets, with values ranging from 8.8 d (for HD 190771) to 22.7 d (for HD 146233). Apart from rotation, fundamental parameters of the selected objects are very close to the Sun's, making this sample a practical basis to investigate the specific impact of rotation on magnetic properties of Sun-like stars.
We reconstruct the large-scale magnetic geometry of the targets as a low-order  (ℓ < 10)  spherical harmonic expansion of the surface magnetic field. From the set of magnetic maps, we draw two main conclusions. (i) The magnetic energy of the large-scale field increases with rotation rate. The increase in chromospheric emission with the mean magnetic field is flatter than observed in the Sun. Since the chromospheric flux is also sensitive to magnetic elements smaller than those contributing to the polarimetric signal, this observation suggests that a larger fraction of the surface magnetic energy is stored in large scales as rotation increases. (ii) Whereas the magnetic field is mostly poloidal for low rotation rates, more rapid rotators host a large-scale toroidal component in their surface field. From our observations, we infer that a rotation period lower than ≈12 d is necessary for the toroidal magnetic energy to dominate over the poloidal component.     

L波段雷达探空高度评估及其质量标识

以美国NCEP FNL分析数据和我国GRAPES_GFS预报数据为背景场,对2016年7月1日-2017年6月30日北京探空站的L波段秒级探空位势高度（探空高度）从观测余差、平均偏差、标准偏差、概率密度分布、峰度系数、偏度系数、相关系数和均方根误差等参数进行误差分析。根据分析结果对探空高度进行质量标识,并根据质量标识的结果再次求解参数,评估质量标识效果。结果表明:探空高度质量较好,无论是基于NCEP FNL还是GRA-PES_GFS,探空高度的误差基本在±5 dagpm以内。探测高层的观测余差平均偏差和标准偏差表明基于GRAPES_GFS的评估优于NCEP FNL的评估。单一个例选取的可疑点和错误点阈值具有误差特征、自适应的特点。     

Study on the Variational Assimilation Technique for the Retrieval of Wind Fields from Doppler Radar Data

This paper introduces a variational assimilation technique for the retrieval of wind fields from Doppler radar data. The assimilated information included both the radial velocity (RV) and the movement of radar echo. In this assimilation technique, the key is transforming the movement of radar echo to a new radar measuring variable- "apparent velocity" (AV). Thus, the information of wind is added, and the indeterminacy of recovering two-dimensional wind only by AV was overcome effectively by combining RV with AV. By means of CMA GRAPES-3Dvar and CINRAD data, some experiments were performed. The results show that the method of retrieval of wind fields is useful in obtaining the construction of the weather system.     

复杂地形区陆面资料对WRF模式模拟性能的影响

本文利用WRF（Weather Research and Forecasting）模式耦合Noah陆面过程模式,对比研究了使用不同精度陆面资料:WRF默认陆面资料、中国1 km分辨率数字高程模型数据集、2006年MODIS（MODerate-resolution Imaging Spectroradiometer）土地利用和植被覆盖度资料,WRF模式对兰州地区冬季气象场模拟结果的差异。结果表明,近地面气温对陆面资料的精度非常敏感,而风场对陆面资料的精度不敏感,WRF模式对气温的模拟效果好于对风场模拟。采用高精度且时效性好的陆面资料后,WRF模拟的近地面气温准确率提高了15.8%,模拟的夜间气温改进幅度较白天大。陆面资料可影响整个边界层温度场分布,准确的陆面资料对提高WRF模式模拟近地面乃至整个边界层气象场至关重要。尽管风速模拟误差较大,但总体上WRF模式能较准确地模拟出研究区的风场演变特征。使用新的陆面资料后WRF模拟的风速误差略有减小,风向误差略有增加。干旱半干旱区冬季数值模拟需要注意土壤湿度初值和模式初始积分时刻对模拟结果的影响。     

A Statistical Study of Rapid Sunspot Structure Change Associated with Flares

We reported recently some rapid changes of sunspot structure in white-light(WL) associated with major flares.We extend the study to smaller events and present here results of a statistical study of this phenomenon.In total,we investigate 403 events from 1998 May 9 to 2004 July 17,including 40 X-class,174 M-class,and 189 C-class flares.By monitoring the structure of the flaring active regions using the WL observations from the Transition Region and Coronal Explorer(TRACE),we find that segments in the outer sunspot structure decayed rapidly right after many flares;and that,on the other hand,the central part of sunspots near the flare-associated magnetic neutral line became darkened.These rapid and permanent changes are evidenced in the time profiles of WL mean intensity and are not likely resulted from the flare emissions.Our study further shows that the outer sunspot structure decay as well as the central structure darkening are more likely to be detected in larger solar flares.For X-class flares,over 40% events show distinct sunspot structure change.For M-and C-class flares,this percentage drops to 17% and 10%,respectively.The results of this statistical study support our previously proposed reconnection picture,i.e.,the flare-related magnetic fields evolve from a highly inclined to a more vertical configuration.     

吴堡矿区横沟井田矿井充水因素评价

吴堡矿区赋存着丰富的煤炭资源,但开采技术条件较复杂,其中水文地质条件复杂是影响煤炭开采的主要不利开采技术条件。本文依据横沟井田勘探资料,较全面地分析了井田水文地质条件,并着重评价了井田矿井充水因素。认为黄河水对横沟井田煤炭开采无影响;奥灰承压水对山西组煤层开采在正常地段不会造成危害,对太原组煤层开采有很大的威胁。并提出太原组煤层能否开采利用,还需进一步作详细地质勘查研究工作。     

南羌塘盆地中-新生代逆冲推覆构造样式及构造应力场特征

新生代印度板块与欧亚板块的持续碰撞挤压,造成南羌塘地块向南逆冲于拉萨地块之上,并在南羌塘地块内部形成了一系列的由北往南的逆冲推覆构造。然而,到目前为止,我们对这些逆冲推覆构造及夹持其间的褶皱变形的结构组成、构造样式、形成时代以及缩短量分布等问题仍存在很大的争议。本文在详细的野外调查基础上,对赛布错-扎加藏布断裂（SZT）,多玛-其香错断裂（DQT）,隆鄂尼褶断带（LF）及南羌塘与中央隆起带分界的肖查卡-双湖断裂（XST）进行了几何学、运动学分析,建立了精细的构造框架。我们认为这些断裂为始新世以来形成的同时期的叠瓦状逆冲推覆;并通过野外褶皱形态,结合层面、节理面、断层面滑动矢量的分析,识别出南羌塘盆地4期构造应力场：1） 代表中特提斯俯冲碰撞阶段的近S-N 向的挤压;2） 中特提斯碰撞后,随着班公湖-怒江缝合带的形成,南羌塘地区构造应力场转为S-N 向的伸展;3） 新生代印度板块向欧亚板块俯冲碰撞,青藏高原进入陆内变形阶段,南羌塘盆地内表现为NE-SW 向的挤压,形成本文提及的一系列逆冲推覆构造;4） 随着高原的持续隆升,约14 Ma南北向裂谷开始活动,应力场转为NWW-SEE 向伸展,形成双湖裂谷系。     

Effects of substorms on the stormtime ring current index Dst

There has been some discussion in recent times regarding whether or not substorm expansive phase activity plays any role of importance in the formation of the stormtime ring current. I explore this question using the K_p index as a proxy for substorm expansive phase activity and the D_st index as a proxy for symmetric ring current strength. I find that increases in D_st are mildly related to the strength of substorm expansive phase activity during the development of the storm main phase. More surprisingly, I find that the strength of D_st during the storm recovery phase is positively correlated with the strength of substorm expansive phase activity. This result has an important bearing on the question of how much the Dst index reflects activity other than that of the stormtime symmetric ring current strength for which it is supposed to be a proxy.