空间科学学报第22卷总目次2002年

第1期太阳微波爆发频谱事件、.、….、、,……..、……..、…。。一种确定模拟的行星际MHD激波局地参数的新方法…..…………… ,………………..向长青刘玉英 傅其骏 宁宗军王敬芳 魏奉思 黄为民 熊东辉（6太阳活动区 R9077引起的强烈吸收事件…………….、…………………………·.… ..、…..胡红桥 刘瑞源 刘勇华 刘顺林 杨惠根 徐中华 佐藤夏雄 山岸久雄（13第22与23周磁静日北京台银河宇宙线周日变化与半日变化特征…….,…..、,…..、、,…………………………………… 乐贵明 叶宗海 龚菊红 黄文…     

基于小波与交叉小波分析的太阳黑子与宇宙线相关性研究

利用小波分析和交叉小波分析方法, 根据太阳黑子数以及Huancayo和Climax两个测站的月均宇宙线数据, 分析了两个测站的月均宇宙线周期变化, 同时利用太阳黑子数R₁₂对Climax站宇宙线流量进行预测研究. 小波分析结果表明, 太阳黑子与宇宙线除存在显著的11年周期外, 太阳活动高年期间还存在1～6个月尺度的周期特性, 在第22太阳周活动高年时还出现了6～8和1～22个月的变化周期; 交叉小波分析结果表明, 在130个月左右的周期上宇宙线与太阳黑子具有显著的负相关性, 并且宇宙线的变化滞后太阳黑子约8个月; 分别采用预测时刻和8个月前的太阳黑子数, 预测相对误差为3.8912%和3.2386%. 本文方法同样适用于估算其他空间天气参量之间的周期和相关性, 提高各种空间天气参量的预测或预报精度.      

1997年1月7-10日广州台站银河宇宙线强度变化特征

1997年1月7－10日的CME事件虽然只引起了中等强度的磁暴，但引起了很强的地球物理效应，这次CME事件影响了银河宇宙线的强度。本文给出了CME在行星际传播期间广州多方向闪烁望远镜观测台站的几个方向记录的银河宇宙线强度变化的特征，并做了简要的分析。     

低平流层温度对银河系宇宙线强度变化的响应

选用芬兰中子堆监测站从lop年7月至1989年3月的宇宙线强度月平均曲线数据,和在相对应期间我国境内海拉尔等4个高空气象观测站的30hPa和100hPa等位势高度上常规气温观测月平均资料,经统计分析,取得初步结果:低平流层气温与银河系宇宙线辐射强度之间呈现负相关的特性;与银河系宇宙线辐射强度峰区和谷区相对应会在低平流层中引起幅值为2-3℃的温度变化;不同纬度观测站所得观测数据表明,上述增温幅值随纬度降低而减少。      

地磁暴前地面宇宙线强度变化Morlet小波特征分析

用Morlet小波变换对Oulu台站和Apatity台站(主要是Apatity台站)1998-2002年间宇宙线静日和地磁暴前的地面宇宙线强度变化特征进行分析，得到：在宇宙线静日期间普遍存在准24h周期变化特征，并且在当地时间0200，1400左右分别出现最小值和最大值；对12个例子的分析可以看到地面宇宙线强度在地磁暴之前l-2天均出现了不同于宇宙线静日期间变化特征，或有小尺度周期出现，或周期变化完全消失，或有异常24h周期变化，这种变化特征在一定程度上可作为地磁预报的先兆特征之一。     

1989年3月大宇宙线暴事件的特征

本文分析了1989年3月一系列大耀斑等离子体抛射引起的宇宙线强度变化的特征.除对中子成分分析外,还对μ介子成分及其各向异性特征作了分析,讨论了宇宙线强度变化与太阳耀斑特性和地磁扰动之间的关系。分析发现,宇宙线的Forbush下降不仅与太阳耀斑的级别、持续时间,以及在日面上的位置有关,而且还与光学耀斑是否伴有强的X射线暴、是否有强的射电爆发,以及是否引起强的地磁暴紧密有关.各向异性分析表明,3月大事件的各向异性明显小于宁静时的各向异性,这可能是因为受到太阳活动强烈调制之后,宇宙线各向异性趋于减小的原因.     

基于ACE飞船观测的银河宇宙线与太阳风变化的统计研究

基于ACE飞船的资料,通过时序迭加方法统计分析了最近两个太阳活动极小年时期（2007.0-2009.0和2016.5-2019.0年）的宇宙线计数与太阳风参数的关系.结果表明,宇宙线的计数受太阳风共转流相互作用区的强烈影响,宇宙线计数变化与快慢太阳风流界面的位置密切相关,例如流界面的穿越通常伴随着宇宙线计数的下降.分析表明,第一时段的具有“雪犁”效应的宇宙线计数下降对应于流界面附近的扩散系数急剧下降,而第二时段的非“雪犁”效应的计数下降可能是由穿越流界面后的扩散系数增大引起的.日球层电流片也与宇宙线计数变化存在一定的相关性,宇宙线粒子在日球层电流片附近存在一定程度的堆积.太阳风对宇宙线的作用机制表明,宇宙线的漂移和扩散效应决定了其在1AU附近的分布变化.      

Millstone地区垂直等效风场的气候学变化

基于1976---2006年美国Millstone非相干散射雷达的电离层观测数据, 分析了美国Millstone地区不同太阳活动条件下, 包括中性风场和电场漂移共同贡献的垂直等效风场的变化特征. 结果表明, Millstone地区的垂直等效风场表现出比较明显的周日、太阳活动和季节变化特征. 晚间垂直向上的等效风较强, 白天等效风较弱, 甚至接近于零. 在不同太阳活动和季节变化条件下, Millstone地区的等效风场都表现出类似的周日变化特征, 低太阳活动条件下, 晚间表现出较大的向上漂移. 这种周日变化和太阳活动变化特征与Millstone地区受到极区热源驱动大气循环的调制以及离子曳力的增减有关. 春季和秋季有相似的幅度和相位变化趋势, 表现出分点对称性; 冬季晚间向上漂移比夏季弱, 且随着太阳活动增强, 差异更加明显, 这再次体现了极区热源驱动大气循环的影响.      

利用地面宇宙线强度变化预报地磁暴方法初步研究

分析了Nagoya宇宙线闪烁体望远镜探测数据的变化特点,定性地探讨了CME可能引起的地面宇宙线的变化特征,通过实例证实了地面宇宙线通量的异常波动是地磁暴发生的重要先兆特征,并且将8 h内宇宙线通量与该时间段内平均通量的偏差D8(t)参数应用到宇宙线数据分析中.通过数据分析与讨论,认为D8(t)参数达到一定阈值是地磁暴的重要先兆特征,但不是充分条件,虚假信号仍占多数;D8(t)参数与太阳质子事件探测结果相结合,对于大地磁暴的预报有较好的效果.      

强磁场扰动对宇宙线调制的统计研究

对1978─1982太阳活动高年时发生的激波、强磁场扰动及激波与强磁场扰动共存这三类事件引起的宇宙线变化进行了统计研究,得到如下结果:(1)激波与强磁场扰动共存时引起的宇宙线强度下降最为显着;只有激波或强磁场扰动时,宇宙线的强度变化相对较小;(2)标志速度间断的激波是产生宇宙线Forbush下降的重要因素;(3)速度间断在强磁场扰动对宇宙线的调制中可能起一个触发的作用。      

1996-2002年太阳耀斑的统计分析

分析了1996-2002年南北半球的太阳黑子相对数和南北半球太阳X射线耀斑级别(简称Imp)≥M1．0的太阳X射线耀斑的特征和不对称性．分析结果表明，南北半球的太阳耀斑活动的程度交替上升，在2001年7月以前北半球的太阳耀斑活动强于南半球，2001年7月开始耀斑活动逐渐以南半球为主．本文还逐月分析了1996—2001年南北半球的耀斑指数．2000年7月为第23周太阳指数最大的一个月，与第23周太阳黑子相对数最大月均值吻合．     

太阳宇宙线在电离层D层中的电离

本文根据带电粒子对D层大气电离的理论,导出了太阳宇宙线在D层的电子产生率Q(h)的表达式,并计算了不同级别的太阳宇宙线事件、不同能谱参数下,Q(h)在极区随高度的分布。结果表明,不同级别、不同能谱的太阳宇宙线事件在极区产生的电离有显著的差别。同一级别,能谱指数γ越大,在较高的高度上电子产生率越大;能谱指数越小,在较低的高度上电子产生率越大。电子产生率的分布曲线出现明显的双峰,一个峰位于60公里左右,另一个峰位于85公里左右。前一个峰主要由太阳宇宙线中质子产生的,后一个峰主要是z≥2的重粒子成分产生的。本文所得结果明显好于Velinov等人的结果。      

Evolution of Dst index,cosmic rays and global temperature during solar cycles 20–23

We have studied conditions in interplanetary space, which can have an influence on galactic cosmic ray (CR) and climate change. In this connection the solar wind and interplanetary magnetic field parameters and cosmic ray variations have been compared with geomagnetic activity represented by the equatorial Dst index from the beginning 1965 to the end of 2012. Dst index is commonly used as the solar wind–magnetosphere–ionosphere interaction characteristic. The important drivers in interplanetary medium which have effect on cosmic rays as CMEs (coronal mass ejections) and CIRs (corotating interaction regions) undergo very strong changes during their propagation to the Earth. Because of this CMEs, coronal holes and the solar spot numbers (SSN) do not adequately reflect peculiarities concerned with the solar wind arrival to 1 AU. Therefore, the geomagnetic indices have some inestimable advantage as continuous series other the irregular solar wind measurements. We have compared the yearly average variations of Dst index and the solar wind parameters with cosmic ray data from Moscow, Climax, and Haleakala neutron monitors during the solar cycles 20–23. The descending phases of these solar cycles (CSs) had the long-lasting solar wind high speed streams occurred frequently and were the primary contributors to the recurrent Dst variations. They also had effects on cosmic rays variations. We show that long-term Dst variations in these solar cycles were correlated with the cosmic ray count rate and can be used for study of CR variations. Global temperature variations in connection with evolution of Dst index and CR variations is discussed.     

Transient variations of vertical total electron content over some African stations from 2002 to 2012

This paper presents the vertical total electron content vTEC variations for three African stations, located at mid-low and equatorial latitudes, and operating since more than 10 years. The vTEC of the middle latitude GPS station in Alexandria, Egypt (31.2167°N; 29.9667°E, geographic) is compared to the vTEC of two others GPS stations: the first one in Rabat/Morocco (33.9981°N; 353.1457°E, geographic), and the second in Libreville/Gabon (0.3539°N; 9.6721°E, geographic). Our results discussed the diurnal, seasonal, and solar cycle dependences of vTEC at the local ionospheric conditions, during different phases of solar cycle in the light of the classification of Legrand and Simon. The vTEC over Alexandria exhibits the well-known equinoctial asymmetry which changes with the phases of the solar cycle; the spring vTEC is larger than that of autumn during the maximum, decreasing and minimum phases of solar cycle 23. During the increasing phase of solar cycle 24, it is the contrary. The diurnal variation of the vTEC presents multiple maxima during the equinox from 2005 to 2008 and during the summer solstice from 2006 to 2012. A nighttime vTEC enhancement and winter anomaly are also observed. During the deep solar minimum (2006–2009) the diurnal variation of the vTEC observed over Alexandria is similar to the diurnal variation observed during quiet magnetic period at equatorial latitudes. We observed also that the amplitude of vTEC at Libreville is larger than the amplitude of vTEC observed at Alexandria and Rabat, indeed Libreville is near the southern crest of the Equatorial Ionization anomaly. Finally, the correlation coefficient between vTEC and the sunspot number Rz is high and changes with solar cycle phases.     

SMY和第21太阳周期间地磁及太阳活动特点的分析

本文比较第17—21太阳周黑子数、地磁A_p指数、各周极大年≥2级耀斑数、磁暴数及第一、二、三大磁暴情况;分析了≥2级耀斑数及磁暴的分布。21周3级耀斑对应磁暴比例低于19、20周,Ⅳ型及米波射电爆发是产生磁暴的重要条件。进一步分析了21周最大磁暴、最大射电爆发引起的磁暴,最严重的电离层短波通讯干扰及有明亮物质抛射的大耀斑、双带大耀斑引起的磁暴等典型例子。最后对SMY期间22个无黑子耀斑作了分析,它们可能引起中小幅度的磁暴。      

Effect of Interplanetary Transients on Cosmic Ray Anisotropic Variations

In the present work the cosmic ray intensity data recorded with ground-based neutron monitor at Deep River has investigated taking into account the associated interplanetary magnetic field and solar wind plasma data during 1981—1994.A large number of days having abnormally high/low amplitudes for successive number of five or more days as compared to annual average amplitude of diurnal anisotropy have been taken as high/low amplitude anisotropic wave train events(HAE/LAE).The amplitude of the diurnal anisotropy of these events is found to increase on the days of magnetic cloud as compared to the days prior to the event and it found to decrease during the later period of the event as the cloud passes the Earth.The High-Speed Solar Wind Streams(HSSWS)do not play any significant role in causing these types of events. The interplanetary disturbances(magnetic clouds)are also effective in producing cosmic ray decreases.Hαsolar flares have a good positive correlation with both amplitude and direction of the anisotropy for HAEs, whereas PMSs have a good positive correlation with both amplitude and direction of the anisotropy for LAEs. The source responsible for these unusual anisotropic wave trains in CR has been proposed.     

“风云一号（B）”卫星探测到的太阳质子事件

我国“风云一号(B)”气象卫星于1990年9月3日发射入轨,该星载有粒子成分监测器,用来探测空间粒子辐射环境,其中包括测量太阳耀斑时产生的太阳质子事件及其重粒子丰度;银河宇宙线异常成分与强度;内辐射带磁异常区的粒子通量及重粒子成分,“风云一号(B)”卫星运行半年来,我们已获取了上述有关的粒子辐射资料,在卫星上获得这些资料在我国尚属首次,本文主要分析观测到的太阳质子事件。     

Ion production and ionization effect in the atmosphere during the Bastille day GLE 59 due to high energy SEPs

The influence of high energy particles, specifically cosmic rays, on atmospheric physics and chemistry is highly discussed. In most of the proposed models the role of ionization in the atmosphere due to cosmic rays is not negligible. Moreover, effect(s) on minor constituents and aerosols are recently observed, specifically over the polar regions during strong solar particle events. According to the recent findings for such effects it is necessary an essential increase of ion production, specifically during the winter period. The galactic cosmic rays are the main source of ionization in the Earth’s stratosphere and troposphere. Occasionally, the atmospheric ionization is significantly enhanced during strong solar energetic particles events, specifically over the polar caps. During the solar cycle 23 several strong ground level enhancements were observed. One of the strongest was the Bastille day event occurred on 14 July 2000. Using a full Monte Carlo 3-D model, we compute the atmospheric ionization, considering explicitly the contribution of cosmic rays with galactic and solar origin, focusing on high energy particles. The model is based on atmospheric cascade simulation with the PLANETOCOSMICS code. The ion production rate is computed as a function of the altitude above the sea level. The ion production rate is computed on a step ranging from 10 to 30?min throughout the event, considering explicitly the spectral and angular characteristics of the high energy part of solar protons as well as their time evolution. The corresponding event averaged ionization effect relative to the average due to galactic cosmic rays is computed in lower stratosphere and upper troposphere at various altitudes, namely 20?km, 15?km, 12?km and 8?km above the sea level in a sub-polar and polar regions. The 24^h and the weekly ionization effects are also computed in the troposphere and low stratosphere. Several applications are discussed.     

第21,22周峰年太阳射电爆发中毫秒级精细结构的分析

本文对第21周的2840MHz及22周峰年的2545MHz，2645MHz和2840MHz波段上所观测到的285个快速事件进行分析，发现两个峰年的快速事件具有多种多样的快速活动（快速精细结构）．它们与耀斑的对应关系也做了统计分析．