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地磁暴的行星际源研究是了解及预报地磁暴的关键因素之一.本文研究了2007-2012年间的所有Dstmin ≤-50 nT的中等以上地磁暴,建立了这些地磁暴及其行星际源的列表.在这6年中,共发生了51次Dstmin≤-50 nT的中等以上地磁暴,其中9次为Dstmin≤-100 nT的强地磁暴事件.对比上一活动周相同时间段发现,在这段太阳活动极低的时间,地磁暴的数目显著减少.对这些地磁暴行星际源的分析表明,65%的中等以上地磁暴由与日冕物质抛射相关的行星际结构引起,31%的地磁暴由共转相互作用区引起,这与以前的结果一致.特别的,在这个太阳活动极低时期内,共转相互作用区没有引起Dstmin≤-100 nT的强地磁暴,同时,日冕物质抛射相关结构也没有引起Dstmin≤-200 nT的超强地磁暴.以上结果表明极低太阳活动同时导致了共转相互作用区和日冕物质抛射地磁效应的减弱.进一步,分析不同太阳活动期间地磁暴的行星际源发现:在太阳活动低年(2007-2009年),共转相互作用区是引起地磁暴的主要原因; 而在太阳活动上升期和高年(2010-2013年),大部分(75%,30/40)的中等以上地磁暴均由日冕物质抛射相关结构引起. 相似文献
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利用西藏高原及其邻区150个地震,西藏台网、四川台网、世界标准台网及在西藏布设的流动台网的 P 波和 S 波观测资料,得出了该地区的地壳和上地幔的 P 波以及 S 波的速度模型:(1)地壳平均厚度70km,可分为明显的两层.上层厚16km,P 波速度5.55km/s,S 波3.25km/s;下层厚54km,P 波速度6.52km/s,S 波3.76km/s;(2)上地幔顶层 P 波速度7.97m/s,S 波4.55km/s.140km 处出现低速层,层厚约55——62km.低速层下的正速度梯度与地幔顶部盖层相差无几. 相似文献
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本文利用30个基准台所记录的238条长周期面波资料,经过适配滤波和分格频散反演,得到中国大陆及邻区147个分格10-105s的纯路径频散,进而反演出青藏高原及邻近地区深至170km的剪切波三维速度结构.研究表明,青藏高原中西部地区和东部地区的地壳平均厚度分别为70±7km和65±7km,地壳平均剪切波速度分别为3.55和3.62km/s,上地幔顶盖平均速度分别为4.63和4.61km/s; 岩石层厚度均为120±10km;东部地区下地壳内30-40km深度处普遍存在低速层;青藏高原及其东侧的上地幔低速层内有横贯东西且明显向上隆起的低速腔.滇西缅北地区的地壳厚45±5km,上地壳及下地壳内都有低速层;上地幔顶盖的速度为4.42km/s,比青藏高原本体及恒河平原都低.恒河平原地壳厚34±2km,速度平均为3.45km/s;上地幔顶盖厚86±10km,速度平均为4.63km/s,顶盖内55-83km深处有一个低速夹层. 相似文献
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2019年8月2日河北省唐山市路南区某矿井区发生ML2.4巷道塌陷,基于塌陷周边台站观测到的短周期瑞雷波,提取面波基阶群速度频散曲线,并利用迭代反演方法得到研究区域地下10 km深度范围内的一维剪切波速度结构,用于精定位分析。速度分析结果表明,研究区域浅表剪切波速度约为2.46 km/s;深度为2 km时,塌陷周边存在小范围的低速区,速度约为2.57 km/s;深度约为4 km时,剪切波速度达3.47 km/s;深度为5～9 km时,唐山东部沉积盆地内存在1个剪切波低速层。精定位分析结果表明,增加浅层速度模型有助于提高深度较小的地震定位精度;塌陷周边的低速区向下延伸近20 km,为地震多发区。 相似文献
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滇西地区地壳上地幔速度结构特征的研究 总被引：47，自引：11，他引：47
本文描述滇西86-87工程资料处理解释的初步结果.结果表明,滇西地区自南向北速度结构有明显的横向不均匀性.莫霍界面深度从剖面南端的38km 加深到北端的58km.地壳的平均速度南低北高,在6.17-6.45km/s 之间.固结地壳为上、中、下三层结构,P10界面是上地壳中的一个弱界面,P20和 P30界面分别是中、上地壳和中、下地壳的分界面,个别地区,在下地壳内部还可以追踪到另一个较弱的 P30界面.PR 界面的深度为0-6km,P10界面的深度为9.2-16.5km,P20和 P30界面的深度分别在17.0-26.5km 和25.0-38.0km 之间.上地壳的速度由南向北逐渐增大,在南高寨与支梯之间达到最大值,基底面的速度可达6.25-6.35km/s,再向北又开始变小.中地壳的速度变化不大,自金河洱海断裂向北中地壳是一速度为6.30km/s 的低速层.下地壳为一较强的梯度层.在剖面南段的景谷与景云桥之间和无量山与澜沧江断裂之间存在-上地幔低速区,Pn 波速度只有7.70-7.80km/s,红河断裂以北 Pn 波速度也低,为7.80km/s.在上地幔顶部还追踪到一个P60界面,剖面南端深65km,北端深85km. 相似文献
7.
《地球物理学进展》1986,(1)
作为多学科考察的一部分,于1978年和1979年,在德国西南都的乌拉赫(Urach)地热异常区进行了地震折射和反射的联合试验,在十条折射测线和两条反射测线上进行了观测记录,测线的最大长度为20—150km不等。根据现有的地震折射资料,本报告提出一个地壳和地幔顶部详细的速度-深度模型。在所有的剖面上、可观测到一个速度为5.6km/s的、清晰的Pg震相,这是来自结晶基底顶部的折射波,在一些剖面上,Pg震相之后有一个逆进的反射波或一个视速度为6.1km/s的潜波,距炮点50km以外,其相应的正进震相的振幅明显地减小,甚至完全消失。这种现象是由一个平均速度为5.8km/s的低速度区引起的,此低速区的深度范围是8—19km,它沿着与施瓦本汝拉山走向平行的主测线在水平方向上延伸一百多公里,低速区的底面由一组反射震相确定,而这组反射震相的品质随反射界面的倾斜程度而变化,该低速区的西部边界在霍恩佐伦地堑的东北缘附近;向东,在内尔特林根里斯的西侧消失。本地区西南部包含此低速区的地壳结构与东北部迥然不同,其莫霍面是倾斜的一级间断面,在西南部深25km,到东北部深26.5km,在地幔顶部,观测到高速度(≥8.4km/s)和强速度梯度,重力研究结果表明,这个低速区是个高密度区,它可能由液态或气态、或部分熔融物质引起,横波的观测结果也支持这一种解释。 相似文献
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用网格频散反演技术计算了155条瑞利面波混合频散数据,将中国大陆分为目前最小分格2°×2°,得到了中国西部及邻区深至80km地壳和上地幔顶部的三维剪切波SV速度结构。结果表明:(1)天山褶皱系地壳平均厚度为54km,上地壳平均速度为3.3km/s,下壳平均速度3.93km/s,上地幔盖层平均速度为4.64km/s,都偏大。北天山壳厚比天山薄,壳和上地幔盖层下均有低速层。(2)塔里木盆地中部地壳厚46km,到其边缘的昆仑山、天山地带壳厚增加到52～55km。壳内无低速层,壳平均速度很低,为3.49km/s,地表有9km的沉积层。(3)青藏高原莫霍面呈凹形,平均壳厚为67km,平均壳速度为3.58km/s。东西端存在壳内低速层,埋深为15～35km。(4)南北带为构造复杂的区域,莫霍面深度具有东高西低,南北两端高、中间低的特点,带内普遍存在壳内低速层。南北带从群速度、速度、莫霍面等深线都可看到明显的横向差异。(5)准噶尔盆地地壳厚47km,无壳内低速层,中地壳不明显。该区呈稳定的大陆壳结构。(6)柴达木盆地在正常速度的中壳顶部有一高速夹层,速度为3.72km/s,厚10km,上顶部埋深14km。 相似文献
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利用新疆及邻区2万多条Pn射线的走时资料,采用层析成像的方法反演该地区上地幔顶部的Pn速度结构.主要结果是:①新疆地区平均h速度为.2km/s,高于中国大陆地区的平均值(.0km/s),速度变化量从-0.3km/s到0.2km/s.②准噶尔盆地是明显的高Pn速度区,高速区与地貌形状吻合较好,最大值达.4km/s;塔里木盆地整体上呈现高速异常二者都可能与盆地是稳定地块、构造活动和变形较弱有关.③在盆地与山脉的交接带即主要的构造活动带,存在较低的Pn速度,可达7.9km/s.④塔里木南缘中部存在一显著的低速区,可能与岩浆活动和构造活动较强有关.⑤上地幔顶部波速各向异性整体上盆地中心较弱,边缘地带较强.新疆南部波速的各向异性可能是因印度板块对欧亚大陆的碰撞使地幔物质向北蠕动的结果. 相似文献
10.
利用中美合作在青藏高原布设的11台 PASSCAL 宽频带数字地震仪记录到的瑞利面波资料,测得青藏高原内不同块体的瑞利面波相速度(周期为10——120s),并反演了不同路径的地壳上地幔 S 波速度结构,发现青藏高原 S 波速度结构的横向变化显著.亚东——安多裂谷带的面波频散与相邻的块体差异最大,温泉至日喀则路径的相速度比其它路径的相速度明显偏高.该路径的地壳平均速度为3.79km/s,比其它路径的地壳平均速度3.40——3.50km/s高得多.青藏高原内不同块体的地壳中均有低速层存在,但低速层的厚度和速度不尽相同.位于北部的松潘甘孜块体。其地壳较薄约为65km,Sn 速度为4.48km/s,而且在约120km 深处的上地幔中存在一厚度为60km,速度为4.15km/s 的上地幔低速层.其它路径的上地幔速度相近,均没有明显的上地幔低速层出现.羌塘块体与拉萨块体的瑞利波相速度和 S 波速度结构极为相似,上地幔顶部的速度较松潘甘孜块体略高.在青藏高原广大地区中,地壳的平均速度低,普遍存在地壳低速层;上地幔顶部的横波速度为4.50——4.65km/s,上地幔中或者没有低速层或者低速层埋藏较深. 相似文献
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The solar wind velocity distribution in the heliosphere is best represented using a v-map, where velocity contours are plotted in heliographic latitude-longitude coordinates. It has already been established that low-speed regions of the solar wind on the source surface correspond to the maximum bright regions of the K-corona and the neutral line of the coronal magnetic field. In this analysis, v-maps on the source surface for Carrington rotations (CRs) 1787-1795, during 1987, have been prepared using the interplanetary scintillation measurements at Research Institute of Atmospherics (RIA), Nagoya Univ., Japan. These v-maps were then used to study the time evolution of the low-speed (\leq450 km s−1) belt of the solar wind and to deduce the distribution of solar wind velocity on the heliospheric current sheet. The low-speed belt of the solar wind on the source surface was found to change from one CR to the next, implying a time evolution. Instead of a slow and systematic evolution, the pattern of distribution of solar wind changed dramatically at one particular solar rotation (CR 1792) and the distributions for the succeeding rotations were similar to this pattern. The low-speed region, in most cases, was found to be close to the solar equator and almost parallel to it. However, during some solar rotations, they were found to be organised in certain longitudes, leaving regions with longitudinal width greater than 30○ free of low-speed solar wind, i.e. these regions were occupied by solar wind with velocities greater than 450 km s−1. It is also noted from this study that the low-speed belt, in general, followed the neutral line of the coronal magnetic field, except in certain cases. The solar wind velocity on the heliospheric current sheet (HCS) varied in the range 300–585 km s−1 during the period of study, and the pattern of velocity distribution varied from rotation to rotation. 相似文献
12.
Geomagnetic disturbances in the Canadian region are compared with their solar and heliospheric sources during the decline phase of solar activity, when recurrent solar wind streams from low-latitude coronal holes were clearly defined. A linear correlation analysis has been performed using the following data: the daily and hourly indices of geomagnetic activity, solar wind velocity, and coronal hole area. The obtained correlation coefficients were rather low between the coronal hole areas and geomagnetic activity (0.17–0.48), intermediate between the coronal hole areas and the solar wind velocity (0.40–0.65), and rather high between the solar wind velocity and geomagnetic activity (0.50–0.70). It has been indicated that the correlation coefficient values can be considerably increased (by tens of percent in the first case and about twice in the second case) if variations in the studied parameters related to changes in the ionosphere (different illumination during a year) and variations in the heliolatitudinal shift of the coordinate system between the Earth, the Sun, and a spacecraft are more accurately taken into account. 相似文献
13.
We investigate the inclinations of heliospheric current sheet at two sites in interplanetary space, which are generated from the same solar source. From the data of solar wind magnetic fields observed at Venus (0.72 AU) and Earth (1 AU) during December 1978–May 1982 including the solar maximum of 1981, 54 pairs of candidate sector boundary crossings are picked out, of which 16 pairs are identified as sector boundaries. Of the remainder, 12 pairs are transient structures both at Venus and Earth, and 14 pairs are sector boundaries at one site and have transient structures at the other site. It implies that transient structures were often ejected from the coronal streamer belt around the solar maximum. For the 16 pairs of selected sector boundaries, we determine their normals by using minimum variance analysis. It is found that most of the normal azimuthal angles are distributed between the radial direction and the direction perpendicular to the spiral direction both at Venus and Earth. The normal elevations tend to be smaller than ≈45° with respect to the solar equatorial plane, indicating high inclinations of the heliospheric current sheet, in particular at Earth. The larger scatter in the azimuth and elevation of normals at Venus than at Earth suggests stronger effects of the small-scale structures on the current sheet at 0.72 AU than at 1 AU. When the longitude difference between Venus and Earth is small (<40° longitudinally), similar or the same inclinations are generally observed, especially for the sector boundaries without small-scale structures. This implies that the heliospheric current sheet inclination tends to be maintained during propagation of the solar wind from 0.72 AU to 1 AU. Detailed case studies reveal that the dynamic nature of helmet streamers causes variations of the sector boundary structure. 相似文献
14.
冕洞是太阳风高速流的源区.当冕洞出现在中低纬区域时,太阳风高速流会扫过地球并引发地球空间环境扰动,如地磁暴和高能电子暴等.在太阳活动周下降年和低年,这种类型的扰动占据主导地位.因此,冕洞高速流的到达时间、峰值时间、峰值强度和持续时间等,是空间天气预报的重要内容.本文基于2010年5月到2016年12月的SDO/AIA太阳极紫外图像以及1AU处ACE和WIND卫星的太阳风观测数据,确定了160个冕洞-太阳风高速流事件,定量计算了他们的特征参数,包括冕洞与太阳风高速流的开始时间、峰值时间、峰值强度和结束时间,分析了各个特征参数的分布规律,对冕洞-高速流之间的关系进行了统计研究,并提出了一种新的预报方法,为基于冕洞成像观测的太阳风高速流的精准预报提供了依据. 相似文献
15.
Wen-Rui Hu 《地球物理与天体物理流体动力学》2013,107(3-4):311-330
Abstract In this paper, the general Mach number equation is derived, and the influence of typical energy forms in the solar wind is analysed in detail. It shows that the accelerating process of the solar wind is influenced critically by the form of heating in the corona, and that the transonic mechanism is mainly the result of the adjustment of the variation of the crosssection of flowing tubes and the heat source term. The accelerating mechanism for both the high-speed stream from the coronal hole and the normal solar wind is similar. But, the temperature is low in the lower level of the coronal hole and more heat energy supply in the outside is required, hence the high speed of the solar wind; while the case with the ordinary coronal region is just the opposite, and the velocity of the solar wind is therefore lower. The accelerating process for various typical parameters is calculated, and it is found that the high-speed stream may reach 800 km/sec. 相似文献
16.
Radio frequency observations of cloud-to-ground lightning (CG) were made in 1999 in Guangdong Province with the broadband
lightning interferometer. In this paper, radiation source locations and electric field waveforms are analyzed for different
types of breakdown events, including the preliminary breakdown of in-cloud activities, the stepped leaders of initial strokes
to ground and activities during and following return strokes. It is shown that the structure and development of lightning
discharges and associated breakdown processes can be reconstructed by using this new type of lightning radiation source location
system. The detectable radiation of lightning was primarily produced by the negative breakdown process. The channel was concentrated
with few branches during the preliminary breakdown stage of CG lightning flashes. The radiation sources appeared generally
at the tip of the channel. During the late period of the stepped leader, the radiation sources were dispersed with branches
extended away from the main channel. The radiation sources were in a certain length segment of the channel and the altitude
of the segment descended along with the propagation of the leader to the ground. During the preliminary breakdown and the
stepped leader of initial strokes to the ground, a sequence of fast negative streamers were observed to start continually
from or farther away the lightning-initiated region and propagate along the developed leader channel, which may supply negative
charge that assisted the leader’s development. The progression speed of fast negative streamers was about ten times faster
than the average speed of lightning channel. 相似文献
17.
J. Gosink 《Pure and Applied Geophysics》1982,120(3):503-526
Dumont d'Urville on the Antarctic coast is an area well known for the presence of strong katabatic winds. Since the austral summer 1979/80 a US-French joint experiment has been investigating the katabatic wind in this region. In early 1980 three automatic weather stations (AWS) were installed along a trajectory from Dome Charlie to Dumont d'Urville. Measurements from these stations include air pressure, temperature, wind speed and direction at ground level only. To supplement these data with information regarding the vertical structure and the advective changes in the katabatic flow, two airborne missions were undertaken in November 1980 along a route from Dome Charlie (Dome C) to Dumont d'Urville.In this paper measurements from these two flights are reported and comparisons made with theoretical models of katabatic flow. The data suggest that equilibrium katabatic flow was not established during these two flights. Downslope acceleration of the wind was particularly marked on 20 November, and a hydraulic jump was encountered in the vicinity of Dumont d'Urville. Relative humidity along the trajectory decreased as the coast was approached consistent with the rapid rise in adiabatic temperature. Simultaneously the absolute moisture content of the air increased indicative of net moisture influx. One source of the moisture increase is the evaporation of blowing snow especially in the intense wind region of the coastal slope near Dumont d'Urville. 相似文献
18.
High-performance computational models are required to make the real-time or faster than real-time numerical prediction of adverse space weather events and their influence on the geospace environment. The main objective in this article is to explore the application of programmable graphic processing units (GPUs) to the numerical space weather modeling for the study of solar wind background that is a crucial part in the numerical space weather modeling. GPU programming is realized for our Solar-Interplanetary-CESE MHD model (SIP-CESE MHD model) by numerically studying the solar corona/interplanetary solar wind. The global solar wind structures are obtained by the established GPU model with the magnetic field synoptic data as input. Meanwhile, the time-dependent solar surface boundary conditions derived from the method of characteristics and the mass flux limit are incorporated to couple the observation and the three-dimensional (3D) MHD model. The simulated evolution of the global structures for two Carrington rotations 2058 and 2062 is compared with solar observations and solar wind measurements from spacecraft near the Earth. The MHD model is also validated by comparison with the standard potential field source surface (PFSS) model. Comparisons show that the MHD results are in good overall agreement with coronal and interplanetary structures, including the size and distribution of coronal holes, the position and shape of the streamer belts, and the transition of the solar wind speeds and magnetic field polarities. 相似文献
19.
R. G. Rastogi 《Annales Geophysicae》1997,15(10):1309-1315
A comparative study of the geomagnetic and ionospheric data at equatorial and low-latitude stations in India over the 20 year period 1956–1975 is described. The reversal of the electric field in the ionosphere over the magnetic equator during the midday hours indicated by the disappearance of the equatorial sporadic E region echoes on the ionograms is a rare phenomenon occurring on about 1% of time. Most of these events are associated with geomagnetically active periods. By comparing the simultaneous geomagnetic H field at Kodaikanal and at Alibag during the geomagnetic storms it is shown that ring current decreases are observed at both stations. However, an additional westward electric field is superimposed in the ionosphere during the main phase of the storm which can be strong enough to temporarily reverse the normally eastward electric field in the dayside ionosphere. It is suggested that these electric fields associated with the V × Bz electric fields originate at the magnetopause due to the interaction of the solar wind and the interplanetary magnetic field. 相似文献
20.
Hao-Jie Huang 《地球表面变化过程与地形》2020,45(15):3943-3954
Particle–turbulence interaction has been a research focus in the field of pneumatic transport, especially in aeolian environments. However, knowledge regarding the effect of saltating particles on the turbulence characteristics is very limited. In this article, a process of sand-laden flow from forming sand streamers to stability is investigated via a coupled mathematical model of wind-blown sand that includes the spatiotemporal development. The variations in the turbulence characteristics, such as the mean velocity and turbulence intensity in clean air or sand-laden flow field, are analyzed. The results show that the splash process of sand grains near the wall decrease the wind speed in the saltation layer and destroy the low-speed streaks. Moreover, the profiles of streamwise turbulence intensity exhibit a transition from ‘decreasing’ to ‘increasing’ and approximately intersect at an ‘intensity focus’, which is presented for the first time. Furthermore, it was found that saltating particles could enhance the Reynolds stress. Meanwhile, it was also noticed that the shear stress at the wall surface is greater than the impact threshold and that there is a tendency towards the impact threshold. Therefore, saltation makes the particle Reynolds number of sand-laden flow higher than that under non-saltation conditions, thus changing the particles’ effect on the turbulence intensity. Gravity-dominated saltation is probably the most essential difference between wind-blown sand and other traditional two-phase flows. © 2020 John Wiley & Sons, Ltd. 相似文献