共查询到20条相似文献，搜索用时 109 毫秒
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本报告依据芬奇和里通1955.0六阶宁静的内源地磁场模式,具体地计算了北京宇宙线台（地理纬度40°02′22″N,地理经度116°11′30″E）的逼近渐近方向、有效垂直截止刚度和变化系数。 相似文献
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安徽南陵NW向第四纪断层的发现及其意义 总被引：1，自引：1，他引：0
在中国东部地区,很难见到错动第四纪地层的断层剖面。在安徽省南陵县南陵至繁昌公路西侧,离南陵县城约2km处(30°55′456″N;118°17′774″E),见到南陵断层错动第四纪地层的剖面,此断裂在卫星影像上有所显示,但是,仅局限于南陵盆地南侧,其西北端终止于小丹阳-方山断裂,长度只有20km,走向NW,断面倾向SW。剖面中,断层由2条小断层组成,至少显示2期活动,第1期在中更新世之前,可能在早更新世;第2期则在中更新世或以后。最新活动为逆冲性质,逆冲位错量有40cm。此剖面显示在中国东部地区NW向断层虽然规模小但活动新 相似文献
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北部湾６级双震的烈度分布魏柏林（广东省地震局，广州５１００７０）１９９４年１２月３１日在北部湾东南（２０°２６′Ｎ，１０９°２８′Ｅ）发生一次Ｍｓ＝６．１级地震。１９９５年１月１０日在原震中附近（２０°３０′Ｎ，１０９°２４′Ｅ）又发生一次６．２级地 相似文献
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中国东部广泛分布着新生代的玄武岩,其地质时代始终是一个争议的问题。本文作者对南京附近地区的两个标准玄武岩组剖面进行了古地磁学研究,使用交变场退磁法检验了样品,证明它们的剩磁稳定性良好,测得江宁方山玄武岩组的I,平均值为8.1×10-4CGSM,Dr=195°29′、Jr=-54°9′,古地磁南极位置为λP=192°35′E、ΦP=76°47′N;六合灵岩山玄武岩组的l,平均值为26.4×10-4CGSM,Dr=354°44′,Jr=42°12′,古地磁北极位置为λP=329°38′E、Φp=80°36′N,并得出如下结论: （1）六合灵岩山玄武岩组和江宁方山玄武岩组的极性截然不同,灵岩山玄武岩组的岩石磁性全系正向,可能相当于布容期（Brunhes epoch）,方山玄武岩组的岩石磁性全属反向,可能相当于松山期（Matuyama epoch）; （2）灵岩山玄武岩组测得的古北极相距现今的北极要比方山玄武岩组的近一些,清晰地表明它们的形成时间绝非同一时期,而是灵岩山玄武岩组要晚,方山玄武岩组要早; （3）灵岩山玄武岩组和方山玄武岩组形成时期的岩石产地所处的古纬度都是中纬度地区,属亚热带气候; （4）对比世界各地区一些有关时代的岩石古地磁学数据,参照这两套玄武岩组的上下地层中所含有的古生物化石及岩石学特征,六合灵岩山玄武岩组的地质时代似应为Q2-Q3,江宁方 相似文献
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Wang Tanwen 《地震地磁观测与研究》1998,19(1):64-67
我国南极中山站、长城站地处极区或靠近极光区,地磁场的变化形态与我国所处的中低纬度地区有所不同,即使是中山站与长城站之间也有较大差异。中山站的暴时ＤＰ型变化就比长城站的明显。重构向量空间吸引子的维数也明显高于北京地区。对长城、中山地磁资料的分析可以扩大我们对地磁场全貌的认识。 相似文献
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用康滇大陆古裂谷带地区航磁异常计算居里深度 总被引：5，自引：2，他引：5
用四川省物探大队1984年编制的1:100万康滇大陆古裂谷带地区航磁异常图,计算该区居里深度。该图包括的面积约60万km2,自东经98°至104°30′,北纬24°至34°。在图上以5km的点距取数,100km×100km的方块作个别分析,每块面积与相邻块相重叠一半。每个块内的数据采用频率域的矩谱法及空间域的线性反演及积分迭代法进行分析计算。为了验证方法的可行性作了理论模型计算。 由计算结果得到该区居里温度等深线图,居里点温度的深度在20km至33km之间。结合大地构造特点及已知地热资料,对图进行了分析。 相似文献
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通过对北极斯瓦尔巴特( Svalbard )岛Longyearbyen台站的 极光扫描光度计和地磁 观测数据在地磁亚暴膨胀相期间的对比分析,发现扫描光度计记录中的极光边缘的快速极向 运动和地磁数据x分量的陡峭负弯之间有着良好的对应关系,地磁数据可用来研究两极 高纬 地区极光亚暴的地磁共轭特征. 对南极中山站、挪威Troms Svalbard台链和东格陵兰岛 地 区共15个地磁台站在7个典型极光亚暴事件中的地磁数据进行对比分析后发现, 中山站的地 磁共轭点位置存在明显的漂移特征,漂移的范围在斯瓦尔巴特岛与东格陵兰岛之间,纬度值 与CGM模型值近似. 相似文献
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行星际激波与地球磁层相互作用通常会导致日侧极光活动增强,随后沿着极光卵的晨昏两侧向夜侧扩展的激波极光.行星际激波也可能直接导致夜侧扇区极光活动增强,甚至沉降粒子能通量的数量级可以与典型亚暴相比拟.本文首次利用我国南极中山站和北极黄河站连续多年积累的极光观测数据,对行星际激波与地球磁层相互作用期间地面台站在夜侧扇区(18—06MLT)观测的极光响应进行了分析.对18个极光观测事件的分析结果表明:行星际激波与磁层相互作用可以在夜侧触发极光爆发和极光微弱增强或静态无变化事件;太阳风-磁层能量耦合的效率以及磁层空间的稳定性决定着行星际激波能否触发极光爆发. 相似文献
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José Manuel Vaquero María Cruz Gallego Fernando Domínguez-Castro 《Geofísica Internacional》2013,52(1):87-92
In recent years, some authors have shown that some auroras can be observed at relatively low latitude when the geomagnetic activity is quiet or moderate. This very special type of aurora is called “sporadic aurora”. We present and analyze in this work a possible case of “sporadic aurora” observed in Mexico on the 19 April 1843. Moreover, we study the solar and auroral activity around this event. 相似文献
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《Journal of Atmospheric and Solar》2008,70(10):1301-1308
The aurora of 4 February 1872 was comparable to, and perhaps even greater than, that of 1/2 September 1859. In this paper we show that the aurora of 4 February 1872 was seen worldwide, and that in the Caribbean, Egypt, Southern Africa, the Indian Ocean, the Indian subcontinent, and China these observations extended as low as 20° magnetic latitude. Observations are also available in the north to as far as the vicinity of the north magnetic pole. This aurora is then comparable to, or greater than, in geographical extent, and in equatorward closeness, to that of 2 September 1859. Both must now be included as the only known members in the class of greatest auroras of the past few hundred years. For the 1859 aurora, however, there is no accepted observation at a lower magnetic latitude than about 20°. By contrast, several observations for the aurora of 4 February 1872 are reported at magnetic latitudes of the order of 10°, and one probable observation at an even lower magnetic latitude of about 3°. This paper presents a survey and discussion of these observations. 相似文献
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Frequently observed throat auroras have been suggested to be correspondent to indentations on the subsolar magnetopause,but how these indentations can be generated is unknown yet.Based on analyzing the detailed observational features of throat aurora,a conceptual model for generation of throat aurora is proposed.This model suggests that precipitation of a north-south aligned stripy diffuse aurora can lead to an ionospheric conductivity enhancement and thus produce a polarization electric field in dusk-to-dawn direction in the ionosphere.After mapping to the magnetosphere along closed field lines,this electric field can guide a magnetopause reconnection to develop inward the magnetosphere and result in a throat aurora.Because this model can comprehensively explain all the observational results that have been presented up to now,we argue that the assumption of ionospheric polarization electric field affecting magnetopause reconnection should be true and be worthy of further investigations. 相似文献
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We document the detailed dynamics of the dayside aurora in the ≈1200–1600 MLT sector in response to a sharp southward turning of the interplanetary magnetic field (IMF) under negative IMF By conditions. Features not documented in previous work are elucidated by using two meridan scanning photometers (separated by 2 h) and an all-sky auroral imager in Ny Ålesund, Svalbard (75.5^MLAT) in combination with magnetograms from stations on Svalbard, covering the latitude range 71^–75^MLAT. The initial auroral response may be divided into three phases consisting of: (1) intensification of both the red (630.0 nm) and green (557.7 nm) line emissions in the cusp aurora near 1200 MLT and ≈100 km equatorward shift of its equatorward boundary, at ≈75^MLAT, (2) eastward and poleward expansions of the cusp aurora, reaching the 1430 MLT meridian after 5–6 min, and (3) east-west expansion of the higher-latitude aurora (at ≈77^–78^MLAT) in the postnoon sector. The associated magnetic disturbance is characterized by an initial positive deflection of the X-component at stations located 100–400 km south of the aurora, corresponding to enhanced Sunward return flow associated with the merging convection cell in the post-noon sector. The sequence of partly overlapping poleward moving auroral forms (PMAFs) during the first 15 min, accompanied by corresponding pulsations in the convection current, was followed by a strong westward contraction of the cusp aurora when the ground magnetograms indicated a temporary return to the pre-onset level. These observations are discussed in relation to the Cowley-Lockwood model of ionospheric response to pulsed magnetopause reconnection. 相似文献
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我们将资源一号卫星星内粒子探测器的观测数据与辐射带模式AE8/AP8的预测结果进行了对比，发现在南大西洋异常区的高能电子和质子的通量与辐射带模型的预测结果基本相同，而在两极极光带的电子通量比AE8模型预测的低得多.根据NOAA卫星的观测结果，可以认为这一差异主要是因为在南大西洋异常区（内辐射带）和两极极光带（外辐射带）的粒子投掷角分布的差异造成的.在南大西洋异常区粒子倾向于各向同性分布，而在极光带粒子各向异性明显，投掷角接近90°的粒子通量比0°投掷角附近的粒子通量大得多. 相似文献
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B. V. Rezhenov 《Annales Geophysicae》1995,13(7):698-703
A mechanism for the formation of aurora connected with the development of an interchange instability on the plasma sheet boundary layer (PSBL) is suggested. The PSBL is assumed to be deep inside the region of closed magnetic field lines. A system of equations connecting currents in the ionosphere and magnetosphere is solved numerically. It is found, using realistic ionospheric and magnetospheric parameters, that in a period of 8–10 min a system of plasma bars directed to the Sun arises at high latitudes. The system of bars is about 1000 km in width and 3000 km in length and approximates the aurora. The suggested mechanism allows an explanation of a number of aurora features such as the appearance probability, electric field directions, energy spectra of precipitating particles, and its location. 相似文献
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《Journal of Atmospheric and Solar》1999,61(3-4):223-232
An active aurora was observed at Eureka, Canada (88.9° N magnetic) following the arrivalat the magnetopause of the shock front resulting from the solar Coronal Mass Ejection of 6January 1997. This onset at 02:20 UT on 10 January marked the beginning of an aurora whichcontinued until at least 15:00 UT on 11 January, as viewed from both Eureka and the CANOPUSsite at Ft Smith (67.8° N magnetic). There were enhanced OI 630 nm polar F-region emissionsthroughout this period, with the IMF Bz controlling their form. When Bz was positive, there were continuous polar arcs; when Bzturned negative there were F-layer patches on open field lines. While the strong Hβ observed over Ft Smith (240 R) in addition to the extended 630 nm emissions and theirpersistence over two days suggested a red aurora of global proportions, it apparently did notextend to latitudes below 60°. There was a moderate magnetic storm associated with the aurora,but the Dst index reached only −81 nT on 10 January. 相似文献