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1.
Characteristics of great geomagnetic storms during solar cycle 23 were statistically investigated. Firstly, we focused on the uniqueness of solar cycle 23 by analyzing both the great storm number and sunspot number from 1957 to 2008. It was found that the relationship between the sunspot number and great storm number weakened as the activity of the storms strengthened. There was no obvious relationship between the annual sunspot number and great storm number with Dstxi≤-300 nT. Secondly, we studied the relationship between the peak Dst and peak Bz in detail. It was found that the condition Bz≤-10 nT is not necessary for storms with Dst≤-100 nT, but seems necessary for storms with Dst≤-150 nT. The duration for Bz≤-10 nT has no direct relationship with the giant storm. The correlation coefficient between the Dst peak and Bz peak for the 89 storms studied is 0.81. After removing the effect of solar wind dynamic pressure on the Dst peak, we obtained a better correlation coefficient of 0.86. We also found the difference between the Dst peak and the corrected Dst peak was proportional to the Dst peak. 相似文献
2.
利用第23太阳活动周中WIND和ACE资料,统计分析行星际扰动对不同水平地磁活动的影响,研究磁暴强度与不同行星际参数之间的相关性,结果发现:①从长期来看,地磁活动指数Dst与太阳风速度的相关性最好,相关性在太阳活动谷年时最高;②多磁暴时序叠加结果证实了导致小、中、强磁暴开始的经验行星际南向磁场条件,磁暴过程中行星际磁场... 相似文献
3.
Relationships between the polar cap magnetic activity index PC and the magnetic storm Dst index have been studied for the magnetic storms with duration more 12 h and peak value Dst<?30 nT and, observed in 1998–2002 and 2004–2005. Along with PC index the geoeffective interplanetary electric field Em was also examined. It has been found that all examined storms, lying in range from ?30 to ?373 nT, started when the PC index and, correspondingly, the Em field firmly exceeded the threshold >2 mV/m. In particular, the “anomalous” magnetic storm on January 21–22, 2005 occurring under conditions of northward IMF BZ (Du et al., 2008) is usual phenomena fitted well with the threshold restriction owing to the large IMF By component input. The maximal storm depression (the peak value of Dst) is linearly related to the quantities Em and PC, averaged for the time interval from the storm beginning to the storm maximum. The correlation between Dst and PC is more steady and larger than correlation between Dst and Em, the latter being dependent on Em value (effect of “Dst saturation”). The moment of the firm descent of the Em and PC quantities below the threshold level ～2 mV/m is indicative of the depression damping and transition to the recovery phase. The results are consistent with the similar peculiarities revealed for substorms development (Troshichev and Janzhura, 2009) and support the conclusion that the PC index is a reliable proxy characterizing the solar wind energy having been entered into the magnetosphere. 相似文献
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A type of relatively low frequency ULF magnetic disturbance has been generally observed by the magnetic induction-meter since
it’s operation at Baijiatuan observatory in Beijing. As the amplitudes and frequencies of such disturbance signals change
with time and are different from the disturbances produced by some man-made magnetic sources, therefore they are usually taken
as a kind of earthquake precursors for ULF electro-magnetic emission. However, a comparative analysis with magnetic storms
on the magnetogram obtained by variometerat the same station indicates that such signals always occur in the period of magnetic
storm occurrence and so far we have not found the cases where such signals occur with no magnetic storms, therefore this kind
of ULF magnetic disturbances should not be taken as a ULF earthquake precursors of the electromagnetic emission at present.
The main features of such signals are as follows: the signals occur discontinuously during storms and the duration of each
time section with such signals and the occurrence rates of the sections and the disturbance amplitudes are usually related
to the types and intensities of storms. The wave form characteristics of the ULF disturbance are also related to the types
of storms. Generally, the amplitudes and durations for SC storms are stronger and longer respectively than those for GC stroms,
and if a storm is with largerK index, then relatively large amplitudes and higher rates and longer durations as well as variable frequencies will be observed
andvice versa. Most of the start time and the time section with strongest disturbance recorded by the ULF unit and by the variometer are
not consistent with each other, and the same one is only about 44%. The periods and intensities of such disturbance signals
are in the ranges of few to several seconds and 0.04–8 nT respectively. The predominant frequency is about 0.06 Hz and certain
energies are also distributed on the harmonic frequencies.
Contribution No. 95A0063, Institute of Geophysics, SSB, China. 相似文献
6.
本文通过对TC-2卫星上搭载的中性原子成像仪(NUADU)在2004年11月发生的一次大磁暴期间观测到的一系列中性原子(ENA)图像的分析,试图给出环电流在磁暴期间的演化模式.研究表明,南向的行星际磁场(IMF)分量在离子从磁尾向内磁层注入和随后的环电流增长过程中起着关键的作用.IMF转为北向后,离子注入随即很快停止.在离子注入增强期间,离子的漂移路径是开放的,以致大量环电流离子从黄昏侧注入后快速地损失在黄昏至正午的磁层顶.所以,环电流往往在离子漂移路径从开放变为封闭后才达到最大强度,而不是在这之前,尽管那时的离子注入强度更大.在该磁暴主相期间,离子注入发生在17∶00~22∶00 LT范围内,形成极其不对称的环电流分布形态.而在恢复相期间,由于受大的IMF By分量的影响,离子注入区的地方时分布范围东向扩张.对称环电流在磁尾对流减小、离子漂移路径变为封闭形态之后形成.在磁暴恢复相后期,从ENA图像看环电流基本衰减到平静时期的水平,而Dst指数仍然显示较强的磁扰动,这说明越尾电流对Dst指数有很重要的影响. 相似文献
7.
本文对南极长城站和北京台1986年1-3月的地磁日变化、磁暴、磁亚暴以及太阳耀斑效应进行了对比分析,不仅获知两地日变化一致和差别的条件,大磁暴和磁亚暴发展过程的全球一致性,而且获得太阳耀斑效应在背阳面也有所反映的有意义结果。 相似文献
8.
对比分析1957--2008年间Dst≤-100nT的强磁暴数与太阳黑子数的变化趋势,发现太阳黑子数和Dst≤-100nT的强磁暴数的变化趋势有很好的一致性。进一步统计强磁暴在太阳周不同阶段的分布后发现,同一太阳周内60％以上的强磁暴出现在下降年,但从太阳周各个阶段的平均磁暴年发生率来看,强磁暴平均年发生率最高的年份仍然是太阳活动极大年。 相似文献
9.
Tan-Wen Wang 《Annales Geophysicae》1996,14(9):888-892
Fractal theory is applied in a quantitative analysis of geomagnetic storms. Fractal dimensions (D) of the attractor for storm data from the Beijing observatory (40.0°N, 116.2°E) using several time intervals are calculated. A maximum value of 1.4 has been obtained for a geomagnetic storm; on quite days the dimension is only slightly larger than 0.5. Data from two storms are analyzed here. Results show that a combination of both D and the magnetic index, k, can perhaps describe the degree of solar disturbance better than the single parameter k. 相似文献
10.
基于CHAMP卫星资料,分析了2002—2008年267个磁暴期间400km高度大气密度变化对季节、地方时与区域的依赖以及时延的统计学特征,得到暴时大气密度变化的一些新特点,主要结论如下:1)两半球大气密度绝对变化(δρa)结果在不同强度磁暴、不同地方时不同.受较强的焦耳加热和背景中性风共同作用,在北半球夏季,中等磁暴过程中夜侧和大磁暴中,夏半球的δρa强于冬半球;由于夏季半球盛行风环流造成的扰动传播速度快,北半球夏季日侧30°附近大气,北(夏)半球到达峰值的时间早于南(冬)半球.而可能受半球不对称背景磁场强度所导致的热层能量输送率影响,北半球夏季强磁暴和中磁暴个例的日侧,南半球δρa强于北半球;春秋季个例中日侧30°附近大气,北半球先于南半球1~2h达到峰值.2)受叠加在背景环流上的暴时经向环流影响,春秋季暴时赤道大气密度达到峰值的时间最短,日/夜侧大气分别在Dstmin后1h和2h达到峰值.至点附近夜侧赤道大气达到峰值时间一致,为Dstmin后3h;不同季节日侧结果不同,在北半球冬季时赤道地区经过更长的时间达到峰值.3)日侧赤道峰值时间距离高纬度峰值时间不受季节影响,为3h左右.在春秋季和北半球冬季夜侧,赤道大气密度先于高纬度达到峰值,且不同纬度大气密度的峰值几乎无差别,表明此时低纬度存在其他加热源起着重要作用. 相似文献
11.
《Journal of Atmospheric and Solar》1999,61(13):993-1000
Hourly equatorial Dst (H) values for a few sudden commencement great geomagnetic storms recorded during the solar cycle 22 are plotted for 72 h of storm time and critically examined. Magnetic records taken at selected low latitude Indian stations are also scrutinised for finer details like SSCs, SIs and other fluctuations. Unusually prolonged main phases lasting more than 20 h characterize the two great storms of 13 March 1989 and 24 March 1991. A second SSC/SI pair, occurring some hours after the first main SSC, has also been identified in these storms. Only the great storm of 28 October 1991, with two SSCs and a main phase duration of 21 h, could be studied in conjunction with simultaneous interplanetary data, including Bz changes. Double negative Bz changes correlate well with the extended and enhanced main phase of this storm. Successive magnetic clouds preceded by interplanetary shock waves could generate such great magnetic storms in association with southward IMF changes. 相似文献
12.
李文静 《地震地磁观测与研究》2021,42(3):109-114
利用磁暴研究地震,特别是预测大地震的报道经常见诸公共媒体,引发诸多质疑。本研究以地震和磁暴(主相最低点)时刻的先后关系为研究对象,在不同时间窗、不同磁暴大小条件下,统计不同震级的地震与磁暴发生之间的时差及对应的地震比例,发现该比例随震前时间窗的增加或磁暴强度的减弱而不断增大,与起始震级基本无关。讨论磁暴对后续地震的"预兆"意义,发现对于中等强度以下的磁暴,在磁暴前后发生的地震比例基本相同,而在强磁暴及更高强度的磁暴后,地震发生概率显著增大,表明强磁暴对地震发生具有一定指示作用。 相似文献
13.
Great magnetic storms (geomagnetic index C9 is ≥8 for St. Petersburg, which can correspond to Kp ≥ 8 or Dst < ?200 nT), registered from 1841 to 1870 at the St. Petersburg, Yekaterinburg, Barnaul, Nerchinsk, Sitka, and Beijing (at the Russian embassy) observatories are analyzed. A catalog of intensive magnetic storms during this period, which includes solar cycles 9–11, has been compiled. The statistical characteristics of great magnetic storms during this historical period have been obtained. These results indicate that high solar activity played a decisive role in the generation of very intense magnetic storms during the considered period. These storms are characterized by only one peak in a solar cycle, which was registered in the years of the cycle minimum (or slightly earlier): the number of great geomagnetic storms near the solar activity maximum was twice as large as the number of such storms during less active periods. A maximum in September–October and an additional maximum in February are observed in the annual distribution of storms. In addition, the storm intensity inversely depends on the storm duration. 相似文献
14.
Seasonal variations in the onset of magnetic storms are investigated. For the purposes of this study storms have been defined as events in which Dst falls below -50 nT for at least four consecutive hours. The storms have been classified as either storm sudden commencements (SSCs; storms initiated by a sudden commencement) or as storm gradual commencements (SGCs; all other storms). It is found that the semi-annual variation of magnetic activity is reflected in the occurrence statistics of SGC events only, indicative that the solar wind origin is different for SSCs and SGCs. It is suggested that the heliospheric latitude model of seasonal magnetic activity is relatively ineffective in modulating the previously observed seasonal variations in the occurrence of magnetic storms. 相似文献
15.
使用TC-1卫星在2004年到2007年磁尾探测数据,将以往高速流的研究拓宽到较低的速度,统计分析其从-13.4RE到-5RE地心距离内的空间演化.研究发现:(1)在向着地球运动的过程中,地向流发生率在日地连线附近减小,但在晨昏两翼的发生率增加,且在黄昏侧的发生率最高;这表明地向流在运动到近地时向着晨昏两翼偏转.(2)越靠近地球,流速V和Vx越小,Vy和Vz的变化幅度较小并且具有明显的晨昏不对称性;所以地向流在近地运动过程中,不仅在晨昏方向上偏转,而且在南北方向上偏转.(3)地向流期间,等离子体密度整体偏小;但是随地心距离的减小,密度整体上逐步增加.(4)平行和垂直于磁场的流速具有明显的晨昏不对称性.在黎明侧的平行流速比黄昏侧大,在黄昏侧的垂直流速比黎明侧大.鉴于较大的垂直流速易触发与电流中断关系密切的不稳定性,我们推测电流中断更容易出现在黄昏侧.(5)除个别位置处的热压和磁压相当外,磁压在总压中一直占据主导地位.日地连线附近的总压较大,晨昏两翼处的总压相对较小;从而在晨昏向上产生较大的压力梯度,导致地向流在晨昏两翼偏转和发生率增大.在晨昏两翼,距离地球较近的位置处观测到了较小的压力;而在日地连线附近,距离地球较远的位置才可以观测到较小的压力;压力分布的这个统计特征说明过去事例研究中电流中断出现在不同的位置可能是由近地磁尾的压力分布造成的. 相似文献
16.
《Journal of Atmospheric and Solar》2000,62(3):157-167
The paper presents a study of solar and magnetic activity effects on VHF ionospheric scintillations recorded during three and half years at Bhopal, a station near the northern crest of the equatorial anomaly in India. During E- (equinox) and D- (winter) months, scintillations occur mainly in the pre-midnight period whereas during J- (summer) months their occurrence is larger in the post-midnight period. Very intense scintillations (>20 dB) mainly occur in the pre-midnight period, and in the post-midnight period, the scintillations are generally moderate (5–10 dB) or weak (<5 dB). The nocturnal scintillation occurrence decreases with the decrease in solar activity from 1989 to 1992. Monthly mean scintillation occurrence changes according to solar activity during E- and D-months but not so during J-months. The effects of magnetic activity on scintillations vary with season and, in general, inhibit the scintillation occurrence in the pre-midnight period and enhance it a little in the post-midnight period, especially after 0300 hours IST (Indian Standard Time). For most of the severe magnetic storms in which Dst goes below −125 nT and the recovery phase starts in the post-midnight to dawn local time sector, strong post-midnight scintillations, which sometimes extend for several hours beyond the local sunrise, are observed. 相似文献
17.
D. V. Blagoveshchensky 《Geomagnetism and Aeronomy》2014,54(5):568-574
Fifty-one magnetic storms occurred during the last solar half-cycle of transition from the epoch minimum to the epoch maximum are considered. Ionospheric (foF2) and magnetic (X component) data from Sodankyla observatory, Finland, were used for the analysis, as well as values of the ΣKp indices of magnetic activity. The dependence of variations in the critical frequency foF2 was studied before, during, and after each storm. It has been revealed that a major effect (ME) takes place for all of the storms analyzed. It consists in the following: the first maximum in foF2 values occurs several days before the onset of the active phase of a storm, then foF2 attains its minimum during the active phase, and the second maximum occurred after the active phase. Five principals, the most frequent types of variation in foF2 during a storm, have been revealed. However, special cases (30%) in which an ME exists but shifts rightward several days along the time axis are observable. Ionospheric “memory” (inertia) from 8–9 h to 2 days has been revealed. It has been ascertained that the occurrence of the first ME maximum can be considered a magnetic storm precursor. Such a precursor potentially can be used for forecasting the beginning of magnetic storm development, which is important for space weather problems. 相似文献
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日冕物质抛射(Coronal Mass Ejection,简称CME)和共转相互作用区(Corotating Interaction Region,简称CIR)是造成日地空间行星际扰动和地磁扰动的两个主要原因,提供了地球磁暴的主要驱动力,进而显著影响地球空间环境.为深入研究太阳风活动及受其主导影响的地磁活动的时间分布特征,本文对大量太阳风参数及地磁活动指数的数据进行了详细分析.首先,采用由NASA OMNIWeb提供的太阳风参数及地磁活动指数的公开数据,通过自主编写matlab程序对第23太阳活动周期(1996-01-01—2008-12-31)的数据包括行星际磁场Bz分量、太阳风速度、太阳风质子密度、太阳风动压等重要太阳风参数及Dst指数、AE指数、Kp指数等主要的地磁指数进行统计分析,建立了包括269个CME事件和456个CIR事件列表的数据库.采用事例分析法和时间序列叠加法分别对两类太阳活动的四个重要太阳风参数(IMF Bz、太阳风速度、太阳风质子密度、太阳风动压)和三个主要地磁指数(Dst、AE、Kp)进行统计分析,并研究了其统计特征.其次,根据Dst指数最小值确定了第23太阳活动周期内的355个孤立地磁暴事件,并以Dst指数最小值为标准将这些磁暴进一步分类为145个弱磁暴、123个中等磁暴、70个强磁暴、12个剧烈磁暴和5个巨大磁暴.最后,采用时间序列叠加法对不同强度磁暴的太阳风参数和地磁指数进行统计分析.统计分析表明,对于CME事件,Nsw/Pdyn(Nsw表示太阳风质子密度,Pdyn表示太阳风动压)线性拟合斜率一般为正;对于CIR事件,Nsw/Pdyn线性拟合斜率一般为负,这可作为辨别CME和CIR事件的一种有效方法.从平均意义上讲,相较于CIR事件,CME事件有更大的南向IMF Bz分量、太阳风动压Pdyn、AE指数、Kp指数以及更小的Dstmin.一般情况下,CME事件有更大的可能性驱动极强地磁暴.总体而言,对于不同强度的地磁暴,Dst指数的变化呈现出一定的相似性,但随着地磁暴强度的增强,Dst指数衰减的速度变快.CME和CIR事件以及其各自驱动的地磁暴事件有着很多不同,因此,需要将CME事件驱动的磁暴及CIR事件驱动的磁暴分开研究.建立CME、CIR事件及地磁暴的数据库以及获取的统计分析结果,将为深入研究地球磁层等离子体片、辐射带及环电流对太阳活动的响应特征提供有利的帮助. 相似文献
20.
用近５０个中纬（磁纬在±２０°-５０°之间）电离层垂测站的ｆ０Ｆ２资料,分析与磁暴相伴的电离层暴事例表明：地磁Ｄｓｔ指数与中纬电离层ｆ０Ｆ２暴时变化Ｄｓ（ｆ０Ｆ２ ）有大致相似的发展趋势。但用时序叠加法求得的强度不同、发展过程和持续时间不同的多次电离层暴ｆ０Ｆ２变化的平均值,其物理意义是很不明确的。暴时ｆ０Ｆ２变化的地方时分布Ｄｓ（ｆ０Ｆ２）中,一般说以全日周期扰动幅度（Ａ１）为最强,但电离层负暴峰值后常出现半日周期扰动（Ａ２）的增强,且有时Ａ２＞Ａ１．Ａ１的涨落趋势与Ｄｓｔ（ｆ０Ｆ２）相似,但特强磁暴时,Ａ１值有可能反而变小．以Ａ１ｓｉｎ（ω ｔ＋ １）表示的全日周期扰动中,初位相１值随暴时的发展而变小表明,扰动分布形态是基本上随地球一起转动的。 相似文献