共查询到19条相似文献，搜索用时 375 毫秒
1.
本文研究了1971－1980年间51个大于3％的宇宙线福布希下降对我国185个气象站上空雷暴活动的短期影响.结果表明，雷暴活动对福布希下降的短期响应存在明显的空间差异．在一些区域中福布希下降后雷暴活动明显增强，而在另一些区域中明显减弱，在这些明显响应区中，雷暴活动在福布希下降前后的差异显著性分别通过了10-2－10－6置信度检验．这些响应区所在的地理位置与雷暴活动对耀斑爆发的响应区相互对应，但响应性质恰恰相反．这些结果给太阳活动与地球短期天气相关机理研究提出了新的挑战，也为进一步的研究提供了新的事实根据． 相似文献
2.
我国雷暴活动对宇宙线福布希下降的短期响应 总被引：2，自引：0，他引：2
本研究了１９７１－１９８０年间５１个大于３％的宇宙线福布希下降对我国１８５个气象站上空雷暴活动的短期影响。结果表明，雷暴活动对福布希下降的短期响应存在明显的空间差异。在一些区域中福布希下降后雷暴活动明显增强，而在另一些区域中明显减弱。在这些明显响应区中，雷暴活动在福布希下降前后的差异显性分别通过了１０＾－２－１０＾－６置信度检验。这些响应区所在的地理位置与雷暴活动对耀斑爆发的响应区相互对应，但 相似文献
3.
本文统计分析了从1976——1985年一个太阳黑子周期期间太阳耀斑爆发和雷暴活动及地面大气电场之间的可能相关性。分析结果指出:(1)耀斑对雷暴活动影响较大,对于高纬度地区二者有较明显的正相关性,相关日在 5日以后。对于2级以上耀斑最大相关日为 7日,增长百分比为18％,且响应变化主要发生在耀斑爆发后 5—— 10日内。中低纬度地区几乎不存在相关性。(2)耀斑强度越强,引起雷暴活动的响应程度越大,且响应区域从高纬度向中低纬度移动。 (3)耀斑爆发后二天左右,地面大气电场明显增大,且随耀斑强度增强而增大。电场强度增大的相关日提前于雷暴数增大的相关日,故雷暴活动增强是大气电场增加的结果,而不是原因。 本文还从全球电路概念出发,简单解释了形成上述相关性的可能原因。太阳活动主要通过对全环大气电路的调制,例如增大大气电场和中层大气电导率等来影响雷暴的起电过程。雷暴中强烈的电活动可以产生和动力涡度相比拟的电涡度,而涡度和上升运动之间存在很强的正反馈过程。因此,雷暴中电活动的加强无疑能促进雷暴的动力发展。目前上述相关性还停留在定性解释上,机制尚不清楚,初步研究发现,雷暴对流起电理论有可能建立上述联系,今后准备利用数值模拟从物理上作定量考察。 相似文献
4.
北京天文台１ ．０２ ．０ＧＨｚ 太阳射电频谱仪从１９９４ 年开始观测至１９９８ 年９ 月记录到太阳射电爆发１７１ 个,２ ．６３ ．８ＧＨｚ 太阳射电频谱仪１９９６ 年９ 月投入观测至１９９８ 年９ 月,记录到１４６ 个太阳射电爆发。１９９８ 年４ 月１５ 日太阳射电爆发同时在这两台频谱仪上记录到。这个事件在时间和频率上显示了丰富的幅度和结构的变化。发现了微波Ⅲ型爆发对群,并存在着丰富的快速活动现象。取得了高时间分辨率、高质量的动态谱资料,为研究耀斑各种尺度的时间及空间演化过程提供了丰富的信息。 相似文献
5.
１９９４年１月５日日面上产生的１次１Ｎ／Ｍ１．０耀斑爆发，射电１．４２ＧＨｚ高时间分辨率观测也同时接收到，在小爆发过程里伴有５３个脉冲信号叠加在连续辐射背景上，是很罕见的现象。在ＡＲ７６４６的黑子前导区域，５日有２处新浮的小黑子对，磁场分别成细小磁流管平行和交又状态，是产生爆发的根源；脉冲信号是微耀斑在射电方面的瞬时辐射现象，由耀斑连续产生微能量释放而出现，单个的能量释放为（０．３—３．３）×１０１０焦耳。在能量释放过程里，非热电子加速起到重要作用。 相似文献
6.
在２２太阳活动周中，日面上有三个较强的质子活动复活体，它们爆发峰值流量≥１００ｐｆｕ和≥１０００ｐｆｕ的质子耀斑各占同类耀斑总数的７０．４％和８３．３％。活动复活体分别位于北纬２６°─３５°和南纬２０°─２９°纬度带上，由于它们周期性（１─２．６年）地再现，从而形成了日面质子耀斑的活动经度和纬度明显集中趋势。 相似文献
7.
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
8.
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
9.
１９９４年１月５日日面上产生的１次１Ｎ／Ｍ１．０耀斑爆发，射电１．４２ＧＨｚ高时间分辨率观测也同时接收到，在小爆发过程里瘵有５３个脉冲信号叠加在连志辐射背景上，是很罕见的现象。在ＡＲ７６４６的黑子前导区域，５日有２处新浮的小黑子对，磁场分别的现象。 相似文献
10.
周树荣 《中国天文和天体物理学报》1996,(3)
本文研究结果表明：同一黑子群在日面期间的顺或反时针方向的旋转运动会先后并存．质子耀斑前1～2无，黑子群的旋转角速度达到极大．耀斑后，磁绳的松弛，黑子群可能会反向旋转，强的剪切过程和质子耀斑可能会再度出现．强质子耀斑活动区的共同特征是：（1）形态为单个团状结构δ型黑子，即众多异极性本影核紧锁在同一黑子半影中；（2）黑子面积＞1000×10－6半球面积，日面跨度＞10°；（3）黑子群都有快速的旋转运动．这类活动区，如果在日面西部活动性明显地增强，那么这个活动区在未来转到日面边缘及其背后、或再次从日面东边缘转出时，定能再次爆发耀斑和伴随较强质子事件。 相似文献
11.
１９９１年５月－６月期间的日面上强质子耀斑的连续爆发,被认为是１９９１年中国江淮特大洪水的重要天文因素。太阳质子耀斑触发和加剧了极涡的冷空气南下,低空西南急流的东移和西太平洋副热带高压的西伸,北抬过程。由于冷暖湿气流在江淮地区频繁地相遇,因此形成了多次暴雨和特大暴雨过程,从而诱发了１９９１年初夏中国江淮流域的特大洪水。 相似文献
12.
The isotopic ratio of 3He/4He, which is routinely measured in the solar wind, on meteorites and in different astrophysical environments, is confined to several times 10-4. However, in impulsive solar flares this ratio reaches often values larger than unity. The evolution of this ratio from the primordial nucleosynthesis to the present solar conditions is sketched and the resonant plasma effects which enhance spectacularly the abundance of 3He in the impulsive solar flares are described. 相似文献
13.
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
14.
The cyclical behaviors of sunspots,flares and coronal mass ejections(CMEs) for 54 months from 2008 November to 2013 April after the onset of Solar Cycle(SC) 24 are compared,for the first time,with those of SC 23 from 1996 November to 2001 April.The results are summarized below.(i) During the maximum phase,the number of sunspots in SC 24 is significantly smaller than that for SC 23 and the number of flares in SC 24 is comparable to that of SC 23.(ii) The number of CMEs in SC 24 is larger than that in SC 23 and the speed of CMEs in SC 24 is smaller than that of SC 23 during the maximum phase.We individually survey all the CMEs(1647 CMEs) from 2010 June to 2011 June.A total of 161 CMEs associated with solar surface activity events can be identified.About 45%of CMEs are associated with quiescent prominence eruptions,27%of CMEs only with solar flares,19%of CMEs with both active-region prominence eruptions and solar flares,and 9%of CMEs only with active-region prominence eruptions.Comparing the association of the CMEs and their source regions in SC 24 with that in SC 23,we notice that the characteristics of source regions for CMEs during SC 24 may be different from those of SC 23. 相似文献
15.
Recent observations have provided much real information about the acceleration of particles in solar flares. High-reliability data about accelerated particles have been obtained for an impulsive phase of some flares of the activity cycle XXII. Therefore, it seems reasonable to re-estimate the amount of Li atoms produced in the upper photospheric layers by – reactions. A value of 5 × 10 29 nuclei during the largest impulsive solar events has been found from calculations for the thick-target model. This agrees with observations of the line of lithium. In conclusion, the probability of enhanced Li absorption observed after large impulsive flares in the sunspot penumbra is discussed. 相似文献
16.
Statistical studies of hard X-ray flares position on the solar disk have shown that the more energetic hard X-rays have a
tendency to be more concentrated near the limb rather than at disk center, whereas lower-energy hard X-ray emission seems
isotropic. Since the high-frequency radio emission is believed to be produced by the same energetic electron population responsible
for the high-energy hard X-rays, we searched the microwave/millimeter emitting bursts for center-to-limb variation in their
emission. A total of 499 bursts observed by the radio telescopes in Bern at the frequencies of 3.1, 5.2, 8.4, 11.8, 19.6,
35.0, and 50.0 GHz were analyzed. Simultaneous Hα flares were used for determination of the radio burst position on the solar
disk. For each of the 7 frequencies, the peak flux and duration were studied as a function of heliocentric position. For 312
bursts, spectral parameters such as spectral index, peak frequency, and flux at spectral maximum were analyzed. For a subset
of 43 bursts with emission at all frequencies, the emission and spectral parameters were analyzed. Center-to-limb variations
of the spectral parameters for all bursts were sought. In order to interpret the observational results, we have performed
a numerical simulation of gyrosynchrotron spectra. We find that high-frequency events, which are also the more energetic ones,
have larger center-to-limb variations in their parameters than do the overall flares. Moreover, this behavior agrees with
theoretical predictions. 相似文献
17.
Previous statistical analyses of a large number of SOHO/MDI full disk longitu-dinal magnetograms provided a result that demonstrated how responses of solar flares to photospheric magnetic properties can be fitted with sigmoid functions. A logistic model reveals that these fitted sigmoid functions might be related to the free energy storage process in solar active regions. Although this suggested model is rather simple, the free energy level of active regions can be estimated and the probability of a solar flare with importance over a threshold can be forecast within a given time window. 相似文献
18.
硬X射线成像是研究太阳耀斑等爆发现象的重要手段.由于采用调制成像而非直接成像的原因, X射线图像在日面上的位置需要借助太阳指向镜提供的仪器指向的日面坐标来确定.因此,指向信息对于耀斑定位实现多波段研究,理解太阳耀斑的物理过程具有重要的科学意义.在此对两种太阳指向镜指向信息的获取算法进行了测试.结合太阳指向镜的设计方案,首先利用SDO (Solar Dynamics Observatory)/AIA (Atmospheric Imaging Assembly) 4500?的数据产生测试图像,其次对其进行二值化处理,分别提取日面轮廓和4个边角指定区域面积;最后分别利用最小二乘法和四象限法对太阳中心坐标进行反演.初步结果显示最小二乘法受随机噪声影响小,定位精度相对稳定约为0.25′′,并可提供四象限法解算的初值;后者的精度可以优于0.14′′,但受随机噪声影响较大.两种算法的精度都显著优于硬X射线成像仪(Hard X-ray Imager, HXI)太阳指向镜的设计要求,可为指向数据在将来科学分析中的实际应用提供参考. 相似文献
19.
We study the occurrence probability of type III radio bursts during flares as a function of the flare position on the Sun. We find that this probability peaks around 30° east of the central meridian, which points to a reciprocal tilt of the average radiation pattern of type IIIs. We argue that anisotropic scattering of the radiation by overdense coronal fibers parallel to the magnetic field is the dominant factor determining the orientation of radiation patterns. It follows that the average magnetic field appears to be tilted 30° west from the vertical. We also find that within a given active region, the average type III production rate of flares peaks 1° west of the center of gravity of all the flares of this active region.We infer that the coronal magnetic field above active regions presents a strong east-west asymmetry, resulting from the well known asymmetry at the photospheric level. As the west side of an active region covers a smaller area with stronger magnetic field than the east side, western flares are generally closer to open field lines than eastern flares. As a consequence, accelerated particles on the trailing (east) side of active regions usually stay trapped in magnetic loops, while on the leading (west) side they are more likely to escape along open lines into interplanetary space. As a result of the initial westward tilt of these open lines, we estimate that the corresponding Archimedean spiral is on average (apparently) rooted 15° west of the flare. 相似文献