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Using the ground observation data at Zhongshan Station of Antarctica during July 13 to 17, 2000, the intense absorption events associated with the activities of the solar active region R9077 are analyzed. It was shown that an intense polar cap absorption event lasted more than 3 days, which was caused by the solar proton event associated with the X5/3B major flare at 1024 UT on July 13. The polar cap event started at about 1040 UT on July 14, and lasted to about 1940 UT on July 17, with a typical day night variation. At the same time, the intense solar activities extremely disturbed the magnetosphere, therefore aurora substorms occurred frequently. The energetic particle precipitation from the magnetosphere caused several absorption spikes superposing on the background of polar cap absorption. One distinct event is the absorption enhancement that started at about 0300 UT on July 15, reached its peak of 26 dB at about 0645 UT and recovered at about 1110 UT on the same day, which was the strongest absorption event observed at Zhongshan Station since the imaging riometer installed in February, 1997. Another outstanding absorption spike with pulsation occurred at about 1753 UT on 14th, its peak reached to 6 dB. 相似文献
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本文利用南极中山站的数字式电离层垂直测高仪１９９５年的频高图资料，对中山站上空冬季电离层的一些平均特性进行了初步分析。中山站冬季电离层Ｆ层很不稳定，其日变化比较明显，ｆｏＦ２的月中值在０９００ＵＴ出现极大并在１４００ＵＴ附近出现次极大。最大值在０９００ＵＴ（磁中午）附近，这是极隙区软电子沉降、极区等离子体对流和光辐射电离效应等诸多因素综合作用的结果，形成了所谓的磁中午异常。在２０００～０１００ＵＴ之间ｆｏＦ２数值较小，可能是由于这段时间中山站正处于电离层极洞区域。Ｅｓ层几乎每天都可以观测到，在１７００ＵＴ附近出现机率较高，并且ｆｏＥｓ数值较大，多数为极光型Ｅｓ，主要是由于极光粒子沉降引起的。电离层Ｅ层的变化相对平缓。 相似文献
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在南极中山站利用甚低频传播手段观测太阳耀斑爆发及极区粒子沉降对低电离层的影响。在一个月的时间里共观测到 6 0次太阳耀斑爆发事件 ,其中最大的一次耀斑爆发引起低电离层等效反射高度下降 8.7公里 ,X射线 (1 - 8A)峰值流量为 3 .5× 1 0 - 2尔格 /(厘米 2·秒 ) ,造成中山站至北京的短波通讯中断 1小时。在这次耀斑爆发 5 8小时以后 ,又观测到在南极地区有粒子沉降事件 ,并引起低电离层等效高度下降 3 .3公里。 相似文献
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20 0 0年 7月 ,太阳表面发生了一系列的耀斑与日冕物质抛射事件 ,最大耀斑能级达X5 .7/3 B。地球表面发生相应特大磁暴 ,Dst指数最大负偏达 - 3 0 0 n T。中国南极中山站地处极隙区纬度 ,白天位于磁层极隙区 ,夜间位于极盖区 ,以多种高空大气物理观测设备详细记录了该磁暴过程。对有关数据的分析表明 ,高能粒子引起电离层吸收急剧增加 ,测高仪数据两天多信号空白 ,宇宙噪声吸收显著增加 ;地磁 Pc3 /5脉动增加与行星际磁场南向分量密切对应 ,显示行星际磁流体波对激发磁层脉动的贡献 ;磁暴主相期间 ,Pc3 /5脉动大幅度增加 ;极区地磁水平分量随南向行星际磁场变化 ,但滞后近 8小时 ;Dst指数与南向行星际磁场密切相关 ,磁暴受控于高度负偏的南向行星际磁场 相似文献
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A series of solar flare and coronal mass ejection (CME) event occurred in July 2000, particularly the largest flare (X5.7/3B) with CME on 14th of July since 1989, which stimulated a great geomagnetic storm with D st index reaching -300 nT. A number of data have been obtained from the Chinese Antarctic Zhongshan Station (ZHS, INT Lat. 74.5°, L≈14), which is located at cusp latitude, and from the ACE satellite. After analyzing these data we have got the results as follows: a lot of solar high energy particles penetrated into the polar ionosphere and ionized it, which significantly increased the cosmic noise absorption (CNA) and blanked the DPS-4 data for more than two days. The magnetic pulsation in Pc 3/5 frequency band on the ground has a high relation with the fluctuation of interplanetary magnetic field (IMF) B z, which shows the contribution of interplanetary magnetohydrodynamical (MHD) waves to the Pc 3/5 pulsation on the ground. The Pc 3/5 pulsation was intensified much during the great magnetic storm. The H component of the magnetic field at ZHS varied with the southern value of IMF B z but lagged behind for about 8 10 h. While D st index responded to the variation of the IMF B z very quickly, which suggested that the magnetic storm occurred at low latitude firstly and then effected the ionospheric current at high latitude. 相似文献
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A polar magnetic substorm on 1974 September 11 was recorded by a two-dimensional array of 25 three-component magnetometers, so located that the westward ionospheric current passed over the array. The mean perturbation fields over five-minute intervals are presented at six representative epochs of the substorm, the first just before its onset and the sixth 21/2 hr later in the coda of the event. At four of the resulting 'time frames', the perturbation fields have been fitted, on a least-squares criterion, by calculated fields of three-dimensional current loops having downward field-aligned current at the east end of the ionospheric westward current, upward field-aligned current at the west end and closure in the magnetotail. The current density was constant across the width of each of these model currents. In three of the four time frames it proved necessary to introduce a bend to the northwest in the ionospheric current; this bend occurred within 27° (geomagnetic) west of geomagnetic midnight. An association with the Harang discontinuity is possible. The field-aligned current nearer to the array (in one time-frame the downward, east-end current, in two others the upward current at the west end) proved essential to secure any reasonable fit to the data. The ionospheric segment of the current loop moved at least 20° of longitude eastward, relative to the surface of the earth, between 07.48 and 08.58 UT. In this 70-min period the ionospheric segment moved at least 38° eastward relative to magnetic midnight. 相似文献
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利用南极中山站和戴维斯站观测的感应式磁力计数据,运用互谱分析方法统计分析了2004年3、6、9、12月的Pc1-2波事件,研究了Pc1-2波出现频次、中心频率和振幅对季节和磁地方时的分布。结果共获得有效Pc1-2波事件2932件,其中,出现在3、9月较多,分别占51.4%和26.1%,12月次之,占18.6%,6月最少,占3.8%。两站的Pc1-2波事件有59.8%出现在磁中午(0800—1000 UT)附近,且在午后靠近磁中午的时候Pc1-2波的中心频率比在午前靠近磁中午的时候大,振幅则在0800 UT时出现最大值;此外,在6月,Pc1-2波的平均中心频率最大,而平均振幅则最小。这些结果表明,极隙区纬度Pc1-2波的传播在很大程度上受电离层电导率的影响。 相似文献
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麦阔里岛和戴维斯站分别位于极光带中心和极光带极向边缘区内.这两处的极光吸收次数在晚间多些,其中突然性吸收主要出现在午夜(当地地磁时间)前,缓变性吸收在午夜后.极光吸收与太阳的活动性密切相关.太阳风高能粒子主要沉降在极光中心带磁午夜区,然后向东西与南北方向扩散,以向西的电射流为主,向东的为辅.但向西的弱些、速度慢些;向东的强些、速度快些.太阳活动增强后,尤其是强的X耀斑事件后,向西的电射流增多增强.另外,在较高磁纬地区的戴维斯站,冬季时极光吸收增多增强.但在极光中心区的麦阔里岛观测站,基本上无此种季节效应.这可能是由于冬季(对南半球而言)极光卵向南偏移造成的. 相似文献
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Post-noon ionospheric absorption observed by the imaging riometers at polar cusp/cap conjugate stations 总被引：1，自引：1，他引：0 
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下载免费PDF全文 An example of post-noon ionospheric absorption observed by the imaging riometers at Ny-Alesund / Danmarkshavn in the arctic region and Zhongshan Station in Antarctic is presented. The post-noon absorption observed simultaneously between the hemispherical stations was a spike-type with weak intensity (<1 dB) during the high solar wind dynamic pressure. The absorption spikes might be caused by precipitation of highrenergy electrons (30 - 300 keV) in the closed dayside magnetosphere. It should be noted that the precipitation region of the absorption spike associated with the steep pressure increase (~ 13 nPa) was localized and shifted equatorward. 相似文献
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本文首次报告了Ｌａｃｏｓｔｅ＆Ｒｏｍｂｅｒｇ－ＥａｒｔｈＴｉｄｅ２１地球潮汐重力仪在南极中山站记录到“不明地学事件”的情况，并对这种有待进一步证实的现象进行了简单描述和初步分析。 相似文献
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Seasonal characteristics of F region in lower solar activity period at Zhongshan Station, Antarctica 下载免费PDF全文
下载免费PDF全文 Based on data of Digisonde Portable Sounder-4 (DPS-4 ) in 1995 -1997. we have analyzed the seasonal variations of F region at Zhongshan Station (69. 4°S,76. 4°E ). During the summer of Zhongshan Station, F region ionization is mainly controlled by the solar ultraviolet radiation. Similar to the phenomena in mid-latitude area, the value f0F2 is changed with local time. During equinox scasons, soft electron precipitation from the cusp/cleft region seems significant, f0F2 is changed with rnagnetic local time, and shows the magnetic noon phenomenon. In winter. the effect of the solar radiation on the F region is less than that of summer. Instead, F region is affected by particle precipitation from cusp/cleft region as well as polar plasma convection, there fore, the diurnal variation of f0F2 is more complex and shows two peaks. F region occurs all day in summer. and seldom appears at midnight in equinox.In winter, F region shows two minimums, one is at midnight and the other is at afternoon cusp. Further analysis of the F region spread indicates that in winter the aurora oval passes over the Zhongshan Station is at 1100 UT - 1500 UT. 相似文献
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利用1999—2011年EISCAT(EISCAT Tromsø UHF)和ESR(EISCAT Svalbard Radar)雷达的场向电子密度观测数据, 对比分析了两处雷达观测到的极区E层占优电离层ELDI (E-Layer Dominated Ionosphere)事件在太阳活动高、低年的统计特征。地面雷达观测表明, 太阳活动水平对极区ELDI发生率的空间分布影响显著: 在太阳活动高年, ELDI在EISCAT雷达处(极光椭圆区纬度)的发生率高于ESR雷达处(极尖/极隙区纬度); 在低年则恰好相反。夏季似乎不利于ELDI的发生, 且在该季节的变化特征不受太阳活动水平及空间位置变化的影响。两部雷达在太阳活动高年观测到ELDI的季节变化规律分别与低年期间的结果相一致: 在冬季和早春, ELDI的发生率较高, 其他季节发生率较低, 夏季尤其低。在ELDI事件期间, 两处雷达观测到事件的持续时间和电离层E层厚度随太阳活动水平的变化表现出明显差异: 高年事件的持续时间总体上比低年短, 低年观测到ELDI的厚度要小于高年结果; 然而NmE/NmF2比值及HmE却没有表现出明显依赖。 相似文献
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Summary. A simplified model of the solar quiet-time ionospheric current system is used to calculate the induced currents in a model earth. The conductivity is assumed to be constant below a depth of about 400 km and zero above that depth. The current induced in the north—south conductivity anomaly under the Rocky Mountains is then estimated from the time-varying potential difference between points at 30 and 45° latitude at the surface of the conducting sphere. The purpose of these calculations is to investigate whether variations in the latitude of the northern hemisphere current system vortex will substantially alter the relationship between the observed magnetic field components at the Earth's surface and the local magnetic field gradient caused by the conductivity anomaly. We find that a 10° shift in the latitude of the ionospheric current focus causes a change of 6 per cent or less in the transfer function from the field components to the gradient in the total field. Thus such latitude shifts cannot explain much of the magnetic field gradient variation at periods near 24 hr that has been observed near Boulder, Colorado. 相似文献
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Risto J. Pirjola Ari T. Viljanen & David H. Boteler 《Geophysical Journal International》2000,140(2):286-294
The relation between the seafloor electric field and the surface magnetic field is studied. It is assumed that the fields are created by a 2-D ionospheric current distribution resulting in the E-polarization. The layered earth below the sea water is characterized by a surface impedance. The electric field at the seafloor can be expressed either as an inverse Fourier transform integral over the wavenumber or as a spatial convolution integral. In both integrals the surface magnetic field is multiplied by a function that depends on the depth and conductivity of the sea water and on the properties of the basement. The fact that surface magnetic data are usually available on land, not at the sea surface, is also considered. Test computations demonstrate that the numerical inaccuracies involved in the convolution method are negligible. The theoretical equations are applied to calculate the seafloor electric fields due to an ionospheric line current or associated with real magnetic data collected by the IMAGE magnetometer array in northern Europe. Two different sea depths are considered: 100 m (the continental shelf) and 5 km (the deep ocean). It is seen that the dependence of the electric field on the oscillation period is weaker in the 5 km case than for 100 m. 相似文献
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《Polar Science》2008,2(3):223-235
In the 44th Japanese Antarctic Research Expedition (JARE-44) during 2003 to 2004, four unmanned magnetometers were deployed in Antarctica to establish a observation network for studying ionospheric and magnetospheric phenomena. Three of them were set about 80 km from Syowa Station, and the fourth was set at Dome Fuji Camp, about 800 km from Syowa. Observations were carried out continuously with a maximum sampling rate of 1 Hz. The purpose of the close network around Syowa was to observe the two-dimensional distribution of the ionospheric equivalent current in a localized area within the field-of-view of the all-sky auroral imager operated at Syowa. Dome Fuji is located at the higher-latitude edge of the auroral zone, while Syowa is located in the middle of it. Auroral observations using the all-sky imager were also carried out at Dome Fuji in 2003. The simultaneous auroral and magnetic observations both at Dome Fuji and Syowa enabled us to study auroral activities in a larger area. This paper describes, the deployment and performance of the unmanned magnetometers in the JARE-44. One auroral substorm event is analyzed in detail to show the usefulness the unmanned magnetometer network. 相似文献
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利用中山站1995-2006年的电离层垂测数据统计分析了当地电离层F2层峰值电子浓度（NmF2）对太阳活动变化的依赖性,研究发现在中山站NmF2月中值随修正太阳10.7厘米通量指数F10.7P增大而增大,其饱和或放大趋势不明显。除冬季12-16 UT、20-2 UT与夏季2-11 UT以外的绝大部分时刻,两者具有良好的线性关系。NmF2月中值随F10.7P变化斜率随季节、地方时而变化。在日变化中,NmF2随F10.7P变化斜率极大值出现在磁中午附近,明显大于其他时刻,在夜侧变化斜率整体较小,且在分季和冬季的夜侧以及夏季全天,其斜率随地方时变化不大。在年变化中,日侧斜率最大值出现在两分季,冬季次之,夏季最小;而夜侧斜率在夏半年（10月-3月）整体上要大于冬半年（4月-9月）。结合中山站位于极隙区纬度的特殊地理位置,分析了上述NmF2变化特征的可能原因。 相似文献