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利用ZH-1(CSES)卫星LAP载荷原位电子密度数据对中国及邻区(0°—54°N,70°—140°E)的顶部电离层背景分布及随季节变化进行了详细分析,研究结果显示:(1)研究区赤道异常的纬度延伸范围、随经度分布形态及它们的季节变化,具有与其他研究结果一致的规律性.(2)中纬度区,白天电子密度存在一个低值带,夜间电子密度呈现高值带.昼夜对比结果显示夜间电子密度升高现象在研究区中纬以上所有季节都存在,但在向低纬延伸时与赤道异常现象呈互补分布,此强彼弱,反之亦然.(3)白天观测的电子密度,半年异常表现为随纬度升高,两峰值出现时间由春秋季向夏季演变,最终过渡到中纬只有夏季峰值的年变形态;季节异常仅在赤道附近4°范围内出现.夜间观测的电子密度,北纬22°以上、50°以下出现半年异常,22°以下出现季节异常.(4)月均值背景总体上表现为夜间电子密度较白天相对波动更剧烈;其中白天电子密度,分季、夏季较冬季波动更剧烈,赤道异常区较中纬区波动更剧烈;夜间电子密度,在所有时、空上波动水平大致相当.(5)研究区电离层背景时空变化特征较为复杂,数据波动亦随时空有变化,对电离层相关科学问题的研究需关注数据背景的分析.综合这些结果及与其他同期观测数据的比较结果,我们认为ZH-1卫星原位电子密度观测数据的相对变化与其他数据集一致.同时,研究区背景数据也呈现了以往研究中未被发现的特征.ZH-1卫星观测数据具有一致的地方时和观测地点,为电离层相关科学问题的系统性研究提供了一个很好的数据集. 相似文献
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本文利用亚洲和美洲地区多个测高仪台站的观测，并结合三维电离层-热层耦合理论模型进行数值模拟，对2020年6月21日和2017年8月21日两次日食事件期间电离层电子密度剖面的变化特征进行分析，并探讨这两次事件中日食效应的异同及形成机制.分析结果表明，在这两次日食期间，位于电离层低高度的E层和F1层的电子密度变化与太阳辐射的变化基本同步；且F1层峰值密度的日食响应幅度大于E层.该结果与以往观测一致，且日食响应无明显的经度变化.进一步地，通过分析观测和模拟结果中电子密度日食衰减效应的高度变化和时延特征，我们发现：(1)观测和模拟结果均表明，食甚时电子密度的最大相对衰减的位置一般不在F1层峰的位置，而是在其上方约几十公里的高度；模拟结果显示该现象是由日食期间F1层上方光化学过程与动力学过程共同作用导致；(2)在中纬地区，在F2层峰附近及以上区域中电离层电子密度最大日食衰减相对太阳辐射变化的时延具有显著的经度变化，其相对衰减在亚洲地区随高度增加而减少，在北美地区随高度无明显变化，与以往报... 相似文献
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利用两颗伴飞的Swarm A/C卫星搭载的双频GPS接收机获取的TEC数据,在两个卫星轨道平面同时对顶部电离层电子密度进行层析成像,实现对顶部电离层电子密度的三维观测.为了能够重现扰动期间电离层电子密度的空间变化特征,在正则化求解过程中,我们引入了水平矩阵H和垂直矩阵V刻画电子密度的空间变化特征,引入整体约束矩阵C以调节不同空间对电子密度相对变化的权重.数值验证结果表明我们的算法对常见的观测误差具有较强的包容性,反演计算出的电子密度平均偏差优于10%.在不同地磁活动条件下,与第三方观测数据的对比,验证了本文反演算法的可靠性.实测数据反演结果表明我们的算法不仅能够较好地重现顶部电离层子午向百公里级别的不规则结构,还能有效分辨纬向相隔~150 km的两个卫星轨道平面的电子密度差异. 相似文献
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《地球物理学报》2020,(9)
利用两颗伴飞的Swarm A/C卫星搭载的双频GPS接收机获取的TEC数据,在两个卫星轨道平面同时对顶部电离层电子密度进行层析成像,实现对顶部电离层电子密度的三维观测.为了能够重现扰动期间电离层电子密度的空间变化特征,在正则化求解过程中,我们引入了水平矩阵H和垂直矩阵V刻画电子密度的空间变化特征,引入整体约束矩阵C以调节不同空间对电子密度相对变化的权重.数值验证结果表明我们的算法对常见的观测误差具有较强的包容性,反演计算出的电子密度平均偏差优于10%.在不同地磁活动条件下,与第三方观测数据的对比,验证了本文反演算法的可靠性.实测数据反演结果表明我们的算法不仅能够较好地重现顶部电离层子午向百公里级别的不规则结构,还能有效分辨纬向相隔～150 km的两个卫星轨道平面的电子密度差异. 相似文献
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本文给出GPS地面台网和掩星观测结合的时变三维电离层层析的原理、算法和基于实测数据的反演结果.反演结果的比较表明,联合地基GPS与掩星观测数据进行重建,电子密度整体图像的重建质量特别是其垂直结构的重建质量得到了明显改善.在平静日和磁暴期间两种条件下利用实测数据的重建结果表明,GPS地面台网和掩星观测结合的电离层层析可以获得电离层电子密度在高度-纬度-经度-时间四维空间中的变化.重建结果清晰地显示了磁暴期间电离层负相暴效应,表明结合GPS地面台网和掩星观测的时变三维电离层层析可以有效地监测扰动条件下的大尺度电离层结构. 相似文献
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本文给出了利用高频天波返回散射雷达对1987年9月23日日环食电离层效应的观测结果.分析表明,日食期间在日环食带电离层存在明显的不均匀结构和小尺度的波动,而日食过后在见食电离层区域出现大尺度的波动现象. 相似文献
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本文给出了利用高频天波返回散射雷达对1987年9月23日日环食电离层效应的观测结果.分析表明,日食期间在日环食带电离层存在明显的不均匀结构和小尺度的波动,而日食过后在见食电离层区域出现大尺度的波动现象. 相似文献
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利用1988～1999年欧洲非相干散射EISCAT（European Incoherent Scatter）雷达观测数据,对不同太阳活动周相、不同季节的极光椭圆区电离层F区电子密度进行统计分析,研究其气候学特征,并与IRI 2001模式比较.EISCAT观测到的电子密度显示出显著的太阳活动高年“冬季异常”和太阳活动低年半年变化等现象.EISCAT实测电子密度随时间和高度的平均二维分布和500 km高度以下总电子含量TEC,从总体来看与IRI 2001模式预测结果符合较好.但高年在TEC达到最大值前后,IRI 2001模式预测的电子密度高度剖面与EISCAT观测结果有显著差别：F2峰以上IRI 2001模式预测的电子密度过大,造成TEC明显高于雷达观测值.另外,在太阳活动下降相,EISCAT观测显示出明显的半年周期季节变化特征,但IRI 2001模式未能预测出此下降相季节变化. 相似文献
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2009年7月22日发生在亚太地区的日全食,从北半球中纬地区一直延伸到南半球中纬地区.这次日食期间发生的磁暴和日食时间同步,使得电离层变化较为复杂.为了分析日食期间电离层扰动及其对定位的影响,所采用的GPS数据来源于日全食带内的重庆CORS网(4个站)、武汉CORS网(8个站)数据、IGS站WUHN、SHAO的数据,以及日偏食区域内不同纬度处的若干IGS站.通过比较日食前后连续三天的各个地方TEC变化,以及利用高采样率的CORS网数据研究日食期间TEC的瞬时变化,根据位置和时间的不同,各地日食期间TEC下降约(1~4)TECU.但是,磁暴期间TEC的响应整体表现为正相暴,偏离值达50%以上,且和日食食甚后的TEC变化相重合.同时,求解了日食期间伪距单点定位的实时精度和CORS网内中短基线的实时精度,伪距单点定位的平面精度变化不显著,高程精度下降达数十米,日食初期CORS网中基线的平面精度仍在厘米级内,高程精度仍在分米级内,但是,日食后期发生的磁暴导致基线的平面精度下降到分米级,高程精度下降到米级. 相似文献
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用120°E经度链附近台站电离层垂测资料和一个二维低纬电离层理论模式探讨1995年10月24日日食电离层效应．在日食条件下只考虑日食区计算太阳EUV辐射减少．模式结果显示：（1）日食期间较低高度电离层光食效应显著,电子浓度跟随食分迅速变化,在食甚后浓度减少达到最大。较高高度电离层对日食响应延迟.（2）低纬地区日食日f0.F2比控制日低,而hmF2比控制日高．在低纬度地区日食带来的影响相对较大·（3）赤道附近hmF2食甚后有一突变,出现日食F1.5层。（4）食甚后海口纬度附近F层受日食影响持久,而f0F2在赤道附近出现第2次下降．最后对低纬日食电离层效应的动力学因素进行了初步的讨论． 相似文献
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The observations of the state of the midlatitude ionospheric D region during the March 29, 2006, solar eclipse, based on the measurements of the characteristics of partially reflected HF signals and radio noise at a frequency of f = 2.31 MHz, are considered. It has been established that the characteristic processes continued for 2–4 h and were caused mainly by atmospheric gas cooling, decrease in the ionization rate, and the following decrease in the electron density. An increase in the electron density on average by 200–250% approximately 70–80 min after the eclipse beginning at altitudes of 90–93 km and approximately 240 min after the end of the solar eclipse at altitudes of 81–84 km, which lasted about 3–4 h, has been detected experimentally. This behavior of N is apparently caused by electron precipitation from the magnetosphere into the atmosphere during and after the solar eclipse. Based on this hypothesis, the fluxes of precipitating electrons (about 107–108 m?2s?1) have been estimated using the experimental data. 相似文献
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E. L. Afraimovich S. V. Voeykov N. P. Perevalova V. V. Vodyannikov G. I. Gordienko Yu. G. Litvinov A. F. Yakovets 《Geomagnetism and Aeronomy》2007,47(4):461-469
The results of studying the ionospheric effects of the March 29, 2006, solar eclipse are presented. The results were obtained in measurements of local electron density (ED) at Alma-Ata vertical ionospheric sounding station and total electron content (TEC) at the Central Asia network of two-frequency receivers of the GPS navigation system. The ED decrease at the F-layer maximum reached approximately 28%, the delay of the minimum value of EC relative to the moment of the eclipse maximum phase was about 11 min, the relaxation time was 4 min, and the duration of the EC depression at the 0.5 level was 45 min. Dynamic interlayer formations were observed in the ionosphere near the eclipse maximum phase. A traveling ionospheric disturbance, probably generated at the shock wave front during the supersonic motion of the Moon’s shadow, was detected. The disturbance period and the horizontal projection of the velocity were about 90 min and ～680 m/s, respectively. The wave vector azimuth (145°) coincides with the model value of the normal to the shock front. 相似文献
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基于低电离层自洽加热模型，综合考虑了低电离层中电子的复合效应及典型吸附效应，本文数值仿真了大功率高频无线电波持续加热低电离层所产生的电子温度、电子密度的扰动，并且首次模拟分析了由于电子温度扰动造成的加热电波自吸收效应.结果表明：电子吸收大功率加热电波能量导致了电子温度的增加，同时改变了电离层的吸收指数，引起了加热电波的自吸收效应.加热电波的自吸收效应对低电离层较高区域的电子温度扰动有重要的抑制作用.因此，随着加热频率的减小或有效辐射功率的增大，低电离层较低区域的电子温度增量明显增大而在高度100 km以上区域的电子温度增量始终较小.另一方面，随着电子温度的增加，电子的复合系数减小而电子的吸附系数增加，导致了电子密度在低电离层中较高区域出现正扰动而在较低区域出现负扰动.当饱和电子温度较大时，继续减小加热频率或增大有效辐射功率对电子密度扰动所造成的改变较小，尤其当电子温度超出复合系数和吸附系数的温度敏感区间.此外，电子温度与电子密度的饱和时间相差较大，电子温度的饱和时间为微秒量级而电子密度的饱和时间为秒量级. 相似文献
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The longest total solar eclipse during the 21st century occurred in South and East Asia on July 22, 2009. Ionospheric response to this rare total solar eclipse which was observed right from the time of sunrise in the Indian zone, has been studied in terms of the total electron content (TEC) obtained from three global positioning system (GPS) receivers located at Udaipur, Hyderabad and Bengaluru, and electron density obtained using space based GPS-Radio Occultation technique. The study reveals significant reductions in the electron density and TEC that persisted up to 2 h past the last contact even during early morning eclipse. These observations imply that during the early morning eclipse, the production and loss of ionization dominate over the plasma transport processes. 相似文献
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This paper presents the results of experimental investigations of variations in maximal usable frequencies (MUFs) during solar eclipses with the use of the method of panoramic tilt sounding by chirps in Eastern Europe and Western Siberia. The characteristics of perturbations of MUFs have been obtained experimentally. It has been established that the effective recombination coefficient increases by 24% in the ionospheric F region with an increase in the maximum eclipse phase from 0.49 to 1.0. 相似文献
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V. V. Belikovich V. D. Vyakhirev E. E. Kalinina V. D. Tereshchenko S. M. Chernyakov V. A. Tereshchenko 《Geomagnetism and Aeronomy》2008,48(1):98-103
The results of observations of the solar eclipse ionospheric effects on March 29, 2006, are presented. The observations were conducted using the partial reflection method near Nizhni Novgorod and the vertical sounding method at the automatic ionospheric station near Murmansk. It has been obtained that the electron density at altitudes of 77 and 91 km decreases by a factor of more than 4; in this case the response of the ionosphere at an altitude of 91 km lags behind the eclipse maximum phase on the Earth by approximately 20 min. It has been established that the eclipse in the E and F1 regions of the polar ionosphere causes a change in the electron density by 15–20%. The delay time of this effect varies from 12 to 24 min depending on the altitude. It has been registered that the reflection virtual altitude at altitudes of the ionospheric F region increases in Murmansk and Nizhni Novgorod. 相似文献
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《Journal of Atmospheric and Solar》2008,70(6):836-853
An annular eclipse occurred over Europe in the morning hours of 3 October 2005. The well-defined obscuration function of the solar radiation during the eclipse provided a good opportunity to study the ionospheric/thermospheric response to solar radiation changes. Since the peak electron density behavior of the ionospheric F2 layer follows the local balance of plasma production, loss and transport, the ionospheric plasma redistribution processes significantly affect the shape of the electron density profile. These processes are discussed here based on a comparison of vertical incidence sounding (VS) and vertical total electron content (TEC) data above-selected ionosonde stations in Europe. The equivalent slab thickness, derived with a time resolution of 10 min, provides relatively good information on the variation of the electron density profile during the eclipse. The computations reveal an increased width of the ionosphere around the maximum phase. As indicated by the available measurements over Spain, the photo production is significantly reduced during the event leading to a slower increase of the total ionization in comparison with the neighboring days. The supersonic motion of the Moon's cool shadow through the atmosphere may generate atmospheric gravity waves that propagate upward and are detectable as traveling ionospheric disturbances at ionospheric heights. High-frequency (HF) Doppler shift spectrograms were recorded during the eclipse showing a distinct disturbance along the eclipse path. Whereas the ionosonde measurements at the Ebro station/Spain in the vicinity of the eclipse path reveal the origin of the wave activity in the lower thermosphere below about 180 km altitude, the similar observations at Pruhonice/Czech Republic provide arguments to localize the origin of the abnormal waves in the middle atmosphere well below the ionospheric heights. Although ionosonde and HF Doppler measurements show enhanced wave activity, the TEC data analysis does not, which is an indication that the wave amplitudes are too small for detecting them via this interpolation method. The total ionization reduces up to about 30% during the event. A comparison with similar observations from the solar eclipse of 11 August 1999 revealed a quite different ionospheric behavior at different latitudes, a fact that needs further investigation. 相似文献