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1.
通过１９９１年６月６日一个复杂的太阳活动事件（包括宽带射电运动Ⅳ型爆发、脉冲相伴生的白光耀斑、耀斑后环及其伴生的射电多重短周期（约１－４劝现象等）的分析,探讨了白光耀斑产生的射电辐射特征,根据太阳白光耀斑和射电运动Ⅳ型爆发产生的物理过程,着重讨论了射电运动Ⅳ型爆发、耀斑后环和短周期脉动现象,并认为它们可能是白光耀斑的对应物。 相似文献
2.
本文对1970年到1979年的太阳中微子流和太阳活动(太阳黑子、耀斑和质子事件)的数据作最大熵谱分析,并求其互相关函数和初相,得到:太阳中微子流和太阳活动均有11年的长周期;太阳中微子流和太阳质子事件还有共同的近3年、2年和1年左右的周期。太阳中微子流的3年周期占支配地位,质子事件中的3年周期亦占有重要地位。二级以上的耀斑事件亦有近两年的周期。它们的互相关函数和初相表明:太阳中微子流与太阳活动有正相关;对近11年周期的数据,太阳黑子和太阳耀斑相对于太阳中微子均有延迟时间47个月,对质子事件有延迟时间41个月。对于约3年的周期,质子的延迟时间为10个月。结合他人的太阳半径和太阳磁场的测量与分析结果,得到一个符合标准太阳模型中物理过程的太阳中微子流变化与太阳活动间的因果关系,并对这个因果关系的可能机制进行了讨论。 相似文献
3.
本文研究了22周中的9个强质子耀斑活动区的共同特征,研究结果表明:单个团状结构黑子,即众多异极性黑子本影核紧锁在同一半影结构中的δ型黑子是强质子耀斑活动区的典型形态特征。黑子群的旋转是质子耀斑活动区的又一重要特征,黑子群的旋转方向与日面南、北半球无关。强质子耀斑的爆发总是在黑子群旋转角度达到正或负相极大之后出现。质子耀斑后,磁绳的松弛,黑子群可能会出现反向旋转,强的剪切过程和质子耀斑可能会再度出现。 相似文献
4.
通过１９９１ 年６ 月６ 日一个复杂的太阳活动事件（ 包括宽带射电运动Ⅳ型爆发、脉冲相伴生的白光耀斑、耀斑后环及其伴生的射电多重短周期（ 约１ － ４ 秒） 脉动现象等） 的分析,探讨了白光耀斑产生的射电辐射特征,根据太阳白光耀斑和射电运动Ⅳ型爆发产生的物理过程,着重讨论了射电运动Ⅳ型爆发、耀斑后环和短周期脉动现象,并认为它们可能是白光耀斑的对应物 相似文献
5.
统计分析了太阳质子事件与微波爆发和软Ｘ射线（ＳＸＲ）耀斑间的关系．结果表明：质子事件的峰值流量与微波爆发和ＳＸＲ耀斑的峰值流量、能通量间呈正的对数线性相关,相关系数０．７—０．８．根据这一统计结果和观测的微波爆发、ＳＸＲ耀斑的有关物理量,可以估算伴随的质子事件峰值流量．太阳质子辐射、ＳＸＲ耀斑和微波爆发三者间的共生关系,可以用磁环中耀斑产生的磁流体动力学过程来解释．大约３３％的质子事件没有对应的Ⅱ型爆发,这表明高能质子的加速有随机ＭＨＤ湍流加速（有Ⅱ型暴）和低频快磁声波湍动加速（无Ⅱ型暴,但有γ射线耀斑）２种不同的加速机制 相似文献
6.
本文对1967—1972年期间的资料较完整的18个质子耀斑活动区,作α因子统计。根据大耀斑区中性线扭曲成“S”形的程度来确定无力场因子α。发现1级以上质子耀斑区,耀斑当天α≥0.34,2级以上,α≥0.50,且耀斑发生前1—2天内α因子均有所增长。因此建议用该α因子预报质子耀斑事件。文中还提出挤压无力场大耀斑模式的设想,以更好地解释一些观测事实。 相似文献
7.
对1970年1月——1973年6月太阳射电观测资料的统计表明,95%的太阳质于耀斑事件,在发生前一天左右,其上空已无米波 f 型源;而当活动区上空存在米波 I 型源时,尽管有特大微波爆发,仍不发生行星际质子事件.另外对典型活动区作的磁势场计算表明,米波 I 型源区的磁结构基本上是封闭的,而质子耀斑区上空,基本上是开放的.这种差别,可能是这两种太阳活动现象彼此排斥的原因. 相似文献
8.
本文对第２２太阳周（１９８７年１月至１９９２年１２月）中发生过Ｍ级以上的Ｘ射线耀斑（Ｈα耀斑级别≥Ｍ级，并伴有Ｘ射线的耀斑）对应的３９５个活动区资料进行了耀斑指数的统计，得到的结果：１．２２太阳周Ｍ级以上Ｘ射线耀斑级别综合指数表，２．２２太阳周Ｍ级以上Ｘ射线耀斑总指数表，３．第２２太阳周Ｍ级以上Ｘ射线耀斑总指数随时间的变化曲线，４．第２２太阳周Ｍ级以上Ｘ射线濯斑总指数直方图，该图表明第２２太阳周活动的极大年分别是１９８９和１９９１年，为第２３周太阳活动预报提供了可用参数。 相似文献
9.
本文在综合分析质子耀斑活动区观测特点的基础上,指出在密集的多极黑子构成的局部区域中,同极黑子分裂,互相排斥,异极黑子相互靠近,向异极区中场强较弱部分的挤压和渗入,是一大批质子耀斑活动区的共同特点.这种黑子间的相对运动,使中性线严重扭曲,呈现出质子耀斑活动区特有的“S”型。根据这些观测特点,寻找到了一种定量估计无力因子的方法。对三个典型的质子耀斑活动区估计了无力因子的变化,并在常无力因子的假定下进行了无力场结构和势场磁能的计算。计算表明质子耀斑发生前无力因子逐渐增加,而势场磁能逐渐减小,减少的势场能量可能正是无力场得到发展的能源,足够质子耀斑的需要。 相似文献
10.
通过对活动区ＮＯＡＡ６８９１中三个Ｘ线耀斑前后的向量磁场分析,研究耀斑发生条件与耀斑发生前后横向磁场和磁剪切变化的关系。我们发现与Ｈａｇｙａｒｄ的耀斑发生条件不同的是,强的横向磁场和磁剪切不是活动区中耀斑发生的充要条件。我们的结果表明,活动区ＮＯＡＡ６８９１ １９９１年３０日的耀斑发生在横向磁场和磁剪切剧烈下降后。尽管１０月２７日的耀斑发生后横向磁场和磁剪切变化很大,但由于有新磁流浮现,造成磁中性 相似文献
11.
M. A. Mosalam Shaltout 《Astrophysics and Space Science》1995,228(1-2):67-75
The year 1991 is a part of the declining phase of the solar cycle 22, during which high energetic flares have been produced by active regions NOAA/USAF 6659 in June. The associated solar proton events have affected the Earth environment and their proton fluxes have been measured by GOES space craft. The evaluation of solar activity during the first half of June 1991, have been carried out by applying a method for high energetic solar flares prediction on the flares of June 1991. The method depends on cumulative summation curves according to observed H-alpha flares, X-ray bursts, in the active region 6659 during one rotation when the energetic solar flares of June 1991 have occurred. It has been found that the steep trend of increased activity sets on several tens of hours prior to the occurrence of the energetic flare, which can be used, together with other methods, for forecasts of major flares. All the used data at the present work are received from NOAA, Boulder, Colorado, USA. 相似文献
12.
我国雷暴活动对太阳耀斑响应的东西不对称性 总被引：3，自引：0，他引：3
本文研究了１９７１—１９８０年间发生在日面东部的１６４个和西部的１３２个２级以上耀斑对我国１８５个气象站上空雷暴活动的影响．结果表明，日面东部耀斑爆发后雷暴活动减弱且通过优于０．１的置信度检验测站数远多于日面西部耀斑，而日面西部耀斑爆发后雷暴活动增强，通过优于０．１的置信度检验测站数远多于日面东部耀斑．这种与地磁活动和日球扰动相似的雷暴活动对太阳耀斑响应的东西不对称性，可能借助于大气电环境并通过行星际磁场和磁层，将太阳和对流层的确耦合起来了． 相似文献
13.
Using the observational data of a Bragg crystal spectrometer on Yohkoh for the period from October 1991 to the end of 1995, we have made a statistical study of flares which consist of a single loop or are dominated by a single loop in SXT images. A total of 158 flares are sampled. With a temporal resolution of three seconds, we conclude that although the blue asymmetry is very common during the impulsive phase, the number of events with total blue shift is rather small, and only a very small number have a large total blue shift, contrasting with the predictions of some hydrodynamic models. It is also found that the blue shift for most flares appears at the early impulsive phase and is temporally correlated with the broadening of the line. These results demonstrate the necessity for checking whether chromospheric evaporation always occurs in solar flares. 相似文献
14.
Y. Hakura 《Solar physics》1974,39(2):493-497
Long-term variation in energetic particle emissivity of the sun was examined by the use of PCA, solar proton flux, and geomagnetic data from 1941 to 1973. A solar cycle may be divided into three periods in terms of the Sun's particle emissivity. The first period with a peak of emissivity coinciding with the maximum of Zurich sunspot numbers is characterized by the random occurrence of proton flares along the heliographic longitude. On the other hand, active centers were restricted in certain longitude regions and had a tendency to produce a series of major flares in a week or two during the second period. The peak of particle emissivity in this period occurred a few years after the first. Relativistic proton events were observed during both the periods of enhanced particle emissivity. In the third period near the end of the solar cycle, MeV proton events of 27-days recurrency became predominating, though particle emissivity of the Sun itself was relatively low. 相似文献
15.
中国地震与太阳活动相关的初步分析 总被引：1，自引：0，他引：1
樊忠玉 《紫金山天文台台刊》1997,16(3):150-155
本文对1934年至1970年的中国地震活动,太阳耀斑活动及质子事件的历史资料进行了初步处理分析,从而发现它们无论从频数或能量变化上都表现出一定的周期性,并探讨了它们之间的关系。 相似文献
16.
We have grouped observed type III solar bursts according to the discrete frequencies of observation in the kilometric wavelength range. For each group we have obtained the bursts' frequency of occurrence as a function of the heliographic longitude of the associated optical flares. We found that flares occurring east of a certain cutoff longitude do not produce bursts observable near the earth below a given frequency. The cutoff on the west is determined by observational limitation for flares beyond the limb. The mean longitude and the extreme eastern end of the longitude distribution both shift to the west as the radio frequency decreases. We interpret these findings in terms of radio wave propagation effects and curved trajectories of the bursts' exciter particles. 相似文献
17.
R. P. Lin 《Solar physics》1970,12(2):266-303
Observations of prompt 40 keV solar flare electron events by the IMP series of satellites in the period August, 1966 to December, 1967 are tabulated along with prompt energetic solar proton events in the period 1964–1967. The interrelationship of the various types of energetic particle emission by the sun, including relativistic energy electrons reported by Cline and McDonald (1968) are investigated. Relativistic energy electron emission is found to occur only during proton events. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. Evidence is presented for two separate particle acceleration and/or emission mechanisms, one of which produces 40 keV electrons and the other of which produces solar proton and possibly relativistic energy electrons. It is found that solar flares can be divided into three categories depending on their energetic particle emission: (1) small flares with no accompanying energetic phenomena either in particles, radio or X-ray emission; (2) small flares which produce low energy electrons and which are accompanied by type III and microwave radio bursts and energetic ( 20 keV) X-ray bursts; and (3) major solar flare eruptions characterized by energetic solar proton production and type II and IV radio bursts and accompanied by intense microwave and X-ray emission and relativistic energy electrons. 相似文献
18.
Kunitomo Sakurai 《Astrophysics and Space Science》1974,28(2):375-519
This paper discusses solar cosmic ray phenomena and related topics from the solar physical point of view. Basic physics of the solar atmosphere and solar flare phenomena are, therefore, considered in some detail. Since solar cosmic rays are usually produced by solar flares, we must first understand the processes and mechanism of solar flares, especially the so-called proton flares, in order to understand the acceleration mechanism of solar cosmic rays and their behaviour in both the solar atmosphere and interplanetary space. For this reason, detailed discussion is given on various phenomena associated with solar flares, proton flare characteristics, and the mechanism of solar flares.Since the discovery of solar cosmic rays by Forbush, the interplanetary space has been thought of as medium in which solar cosmic rays propagate. In this paper, the propagation of solar cosmic rays in this space is, therefore, discussed briefly by referring to the observed magnetic properties of this space. Finally, some problems related to the physics of galactic cosmic rays are discussed.Astrophysics and Space Science Review Paper. 相似文献
19.
《Chinese Astronomy and Astrophysics》1983,7(2):124-129
Starting with the quasi-linear equation of the distribution function of particles in a regular electric field, a combined diffusion coefficient in the momentum space conbining the effects of the regular field and a turbulent field is obtained and a combined mechanism of acceleration by the regular and turbulent fields in the neutral sheet of solar proton flares is proposed. It is shown by calculation that conditions in solar proton flares are such that the charged particles can be effectively accelerated to tens of MeV, even ~1 GeV. It is shown that the combined acceleration by a regular electric field and ion-acoustic turbulence pumps the protons and other heavy ions into ranges of energy where they can be accelerated by Langmuir turbulence. By considering the combined acceleration by Langmuir turbulence and the regular electric field, the observed spectrum of energetic protons and the power-law spectrum of energetic electrons can be reproduced. 相似文献
20.
日冕物质抛射与共生射电爆发的地面和空间联测研究 总被引：1，自引：0，他引：1
引述了近年来太阳和空间物理的一大研究成果；产生日地空间射电爆发和地球物理响应的主因不是太阳耀斑，而是日冕物质抛射（CME），论述了射电爆发在研究CME中的作用；分析了1991-06-15CME事件中射电爆发和质子事件产生的物理过程；介绍了地面/空间对CME和共生射电爆发联测研究的新进展；提出了我国今后开展地面/空间联测研究的设想和建议。 相似文献