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61.
Nishant Mittal Kumud Pandey Udit Narain S. S. Sharma 《Astrophysics and Space Science》2009,323(2):135-145
We have investigated properties such as speed, angular width, location, acceleration and occurrence rate of narrow CMEs (defined
as having angular width ≤20°) observed during 1996–2007 by SOHO/LASCO. The results obtained are compared with those of normal
CMEs (angular width >20°) from the same time interval to find whether there are any real differences between the two populations.
Our study of 3464 narrow CMEs from the online SOHO/LASCO, CME catalogue leads us to conclude that (1) the fraction of narrow
CMEs during solar minimum is 38% and during solar maximum 19%, (2) during solar maximum narrow CMEs are generally faster than
normal CMEs, (3) the maximum speed of narrow CMEs is much smaller than that of the normal CMEs, (4) during solar maximum narrow
CMEs appear at all latitudes similar to normal CMEs, (5) narrow and normal CMEs have unequal deceleration and (6) the occurrence
rate of narrow CMEs remain constant after 1998 until the beginning of 2006 while the normal CMEs occurrence rate seems to
follow solar cycle variation until 2004. Thus narrow CMEs and normal CMEs have some differences, in disagreement with previous
studies. 相似文献
62.
Coronal Mass Ejections (CMEs) are challenging objects to detect using automated techniques, due to their high velocity and
diffuse, irregular morphology. A necessary step to automating the detection process is to first remove the subjectivity introduced
by the observer used in the current, standard, CME detection and tracking method. Here we describe and demonstrate a multiscale
edge detection technique that addresses this step and could serve as one part of an automated CME detection system. This method
provides a way to objectively define a CME front with associated error estimates. These fronts can then be used to extract
CME morphology and kinematics. We apply this technique to a CME observed on 18 April 2000 by the Large Angle Solar COronagraph
experiment (LASCO) C2/C3 and a CME observed on 21 April 2002 by LASCO C2/C3 and the Transition Region and Coronal Explorer (TRACE). For the two examples in this work, the heights determined by the standard manual method are larger than those determined
with the multiscale method by ≈10% using LASCO data and ≈20% using TRACE data. 相似文献
63.
Accompanied by flares and coronal mass ejections, the symbiotic coronal and interplanetary fast shock waves have become a hot topic in particle acceleration. Under the condition of quasi-parallel propagation, we construct a numerical method of solving one-dimensional transport equation, and thereby exploring the physical relationships between the distribution of the accelerated ions and the parameters of the shock waves and background plasmas. Considering the diffusive coefficient as a constant and a function of energy, respectively, the results of calculations of finite free escape boundaries show that (1) the energetic particles approximately exhibit a double power-law distribution and the spectral index decreases gradually from 10.2 to 2.4 in the low energy region of 3-10MeV with the increase of the acceleration time; (2) with the increase of the compression ratio of the shock from 2 to 4, the spectral index decreases from 3.2 to 2.2 at a given time and in the same energy range; (3) when the finite upstream and downstream escape boundaries decrease from 5 to 2, the spectral index of the particle energy spectrum increases from 2.4 to 3.3, and the acceleration efficiency of particles decreases; (4) the spectral index decreases from 2.4 to 0.9 with the increase of the initial inject energy of the particles; (5) when the diffusive coefficient is directly proportional to the energy of the particles, the spectral index increases from 2.2 to 4.3 as compared with the case of constant diffusive coefficient. 相似文献
64.
利用色球Hα、TRACE／WL、SOHO／EITEuV单色像观测资料及SOHO／MDI光球磁场观测资料，对2003年10月22日太阳活动区AR0484内发生的日浪事件进行了研究．发现：(1)在Ha线心观测上，日浪包含有亮、暗2个分量，这2个分量先后出现而且并不共空间．日浪的亮分量与UV和EUV波段上观测到的喷发具有较好的同时性和共空间性．(2)日浪喷发物质沿着EUV环运动。(3)在光球层，日浪足根处的黑子和磁场有明显的变化．这些观测结果支持日浪的磁重联模型。 相似文献
65.
日冕物质抛射(ChIEs)经常被观测到和其他日面活动相伴生，太阳耀斑、日珥爆发、盔状冕流等许多太阳现象，都与它有直接或间接的关系。射电观测是研究CMEs的一种重要的补充工具。多频率的射电成像观测能很好地研究CMEs的初始阶段，而且可以得到关于CMEs触发机制特征的更多信息。概括了CMEs与低频射电的关系，介绍了低频射电的观测仪器，分析了CMEs低频射电所表现出来的特征，考虑了CMEs的初发机制，总结了尚待解决的问题，表明了CMEs研究是基于多类数据和全电磁辐射波段的。 相似文献
66.
Combining the observations of STEREO satellites with the method of three-dimensional magnetohydrodynamic (MHD) numerical simulation, adopt- ing the magnetic ?eld data of the Wilcox Solar Observatory (WSO) and the model of potential ?eld source surface to build up the initial magnetic ?eld in solar corona, and adding a time-varying disturbance of pressure to the active re- gion on the solar surface, the study on the event of coronal mass ejection (CME) and extreme-ultraviolet (EUV) wave happened at 05:35 UT of 2009 February 13 has been performed. It is judged from the images of COR1/STEREO-A that the front speed of this CME is about 350 km·s−1, and the angular width is about 60°. By analyzing the running difference images of EUVI/STEREO-B at 195 ?A, it is found that the bright toroidal wavefront is spreading toward all directions around the active region, and behind the bright toroidal wavefront is a coronal dimming area. The positions of the wavefront in four directions are taken to perform linear ?ttings, it is known that the EUV wave speed is 247 km·s−1, and the EUV wave speed obtained from the numerical simulation is 245 km·s−1. After the IDL visualization program has been carried out for the calculated result, the structures of the bright loop and dimming area can be seen clearly. The numerical simulation is consistent with the satellite observation, which shows that the observed EUV wave may belong to the fast magnetosonic wave. 相似文献
67.
Guan-Nan Gao ;Min Wang ;Jun Lin ;Ning Wu ;Cheng-Ming Tan ;Berhard Kliem ;Yang Su 《中国天文和天体物理学报》2014,(7):843-854
A solar radio burst was observed in a coronal mass ejection/flare event by the Solar Broadband Radio Spectrometer at the Huairou Solar Observing Station on2004 December 1. The data exhibited various patterns of plasma motions, suggestive of the interaction between sunward moving plasmoids and the flare loop system during the impulsive phase of the event. In addition to the radio data, the associated whitelight, Hα, extreme ultraviolet light, and soft and hard X-rays were also studied. 相似文献
68.
日冕物质抛射（ＣＭＥ） 是一个极为复杂的动力学过程本文基于开放场、闭合场的物理条件及射电爆发理论, 研究了ＣＭＥｓ 与相伴随的射电Ⅱ型、Ⅲ型、Ⅳ型爆发、软χ射线增强及太阳耀斑的关系给出了它们相伴随的条件： 当磁通量喷发, 能量释放时, 等离子体将被加速如果加速区在开放场, 可能会产生Ⅲ型爆发; 如果是闭合场, 被加速的高能质子和高能电子将被磁环捕获高能质子在磁环腿部呈损失锥分布, 当Ｅ≥ＥＴ 时会产生软χ射线增强随着磁环内的热压Ｐ和磁压Ｐｍ 的升高, 当β≥βＴ 时, 磁环将炸裂, 产生ＣＭＥｓ抛射出的高能相对论电子绕开放场线作螺旋飞行时, 会产生Ⅳ型爆发; 而亚相对论电子以零入射角沿开放磁场线逃逸时, 会产生Ⅲ型爆发高速飞行的等离子体产生激波时, 会产生Ⅱ型爆发当ＣＭＥｓ 源接近耀斑时, 会触发耀斑爆发 相似文献
69.
文中选了５ 个典型活动区, 分析了这些活动区的磁场, 与活动区相应的ＣＭＥｓ, 太阳爆发事件和太阳质子事件我们发现, 对于Ｅ ≥１０ｍｅＶ 的太阳质子事件有相应的源活动区, 源耀斑和ＣＭＥ; 活动区矢量磁场有剪切, 磁场剪切越强质子事件越强; 多数在质子耀斑发生前出现磁流浮现; 太阳１０ｃｍ 射电爆发持续时间长文中结果还佐证了Ｓｈｅａｌｙ 等的结果： Ｘ 射线耀斑的长持续时间与ＣＭＥ 的发生正相关另外,在５ 个活动区中, 有三个大耀斑发生前没有明显的磁剪切作为它们的先兆, 它们是非质子源耀斑这是Ｍｏｏｒｅ, Ｈａｇｙａｒｄ 和Ｄａｖｉｓ 的磁场强剪切是耀斑产生的必要条件的反例 相似文献
70.
莱曼阿尔法太阳望远镜(LST)是先进天基太阳天文台(ASO-S)卫星的载荷之一,它包括白光太阳望远镜(WST),全日面太阳成像仪(SDI)和日冕仪(SCI)等仪器. 1991年Kuhn, Lin和Loranz提出的方法(简称KLL方法)是WST和SDI在轨平场定标的方法之一.为了研究WST和SDI的平场定标精度对KLL方法的相邻位置时间间隔的敏感性,使用太阳动力学观测卫星(SDO)的日震和磁成像仪(HMI)及太阳大气成像仪(AIA)的全日面成像观测数据测试和分析在使用KLL方法时相邻位置时间间隔对所得平场精度的影响.结果显示在LST使用KLL方法进行平场定标时,相邻位置时间间隔越短越好.具体分析表明,WST平场精度对相邻位置采样时间间隔不敏感,而SDI时间间隔需要在240 s范围内.分析结果对卫星姿态调整到稳定所需的时间给出了一定限制. 相似文献