We explore the link between solar energetic particles (SEPs) observed at 1 AU and large-scale disturbances propagating in the solar corona, named after the Extreme ultraviolet Imaging Telescope (EIT) as EIT waves, which trace the lateral expansion of a coronal mass ejection (CME). A comprehensive search for SOHO/EIT waves was carried out for 179 SEP events during Solar Cycle 23 (1997-2006). 87% of the SEP events were found to be accompanied by EIT waves. In order to test if the EIT waves play a role in the SEP acceleration, we compared their extrapolated arrival time at the footpoint of the Parker spiral with the particle onset in the 26 eastern SEP events that had no direct magnetic connection to the Earth. We find that the onset of proton events was generally consistent with this scenario. However, in a number of cases the first near-relativistic electrons were detected too early. Furthermore, the electrons had in general only weakly anisotropic pitch-angle distributions. This poses a problem for the idea that the SEPs were accelerated by the EIT wave or in any other spatially confined region in the low corona. The presence of weak electron anisotropies in SEP events from the eastern hemisphere suggests that transport processes in interplanetary space, including cross-field diffusion, play a role in giving the SEPs access to a broad range of helio-longitudes.
Interaction of Fast Magnetoacoustic Wave with the Localized Coronal Null and Generation of the Energetic Alfvén Wave Packet
Indian Institute of Technology (BHU)（印度理工学院（贝拿勒斯印度教大学））；Institute of Physics University of Graz（格拉茨大学物理研究所）；Department of Astronomy and Astrophysics at Space Research Center, Ilia State University（伊利亚州立大学空间研究中心天文学与天体物理学系）；Evgeni Kharadze Georgian National Astrophysical Observatory（叶夫根尼·哈拉泽格鲁吉亚国家天文台）；Key Laboratory of Solar Activity and Space Weather, School of Aerospace, Harbin Institute of Technology, Shenzhen（哈尔滨工业大学深圳航天学院太阳活动与空间天气重点实验室）；Korea Astronomy and Space Science Institute（韩国天体与空间科学研究所）
On the Relationship between Solar Spicules and Propagating Coronal Disturbances: The Role of Shocks
Udaipur Solar Observatory, Physical Research Laboratory（乌代浦尔太阳观测台，物理研究实验室）；Indian Institute of Technology, Gandhinagar（印度理工学院，甘地纳加尔）；Indian Institute of Astrophysics（印度天体物理研究所）；Pondicherry University（本地治里大学）；School of Science, University of Newcastle（纽卡斯尔大学理学院）；Solar Physics and Space Plasma Research Centre (SP2RC), School of Mathematical and Physical Sciences, University of Sheffield（谢菲尔德大学数学与物理科学学院太阳物理与空间等离子体研究中心）；Department of Astronomy, Eötvös Loránd University（罗兰大学天文系）；Gyula Bay Zoltán Solar Observatory (GSO), Hungarian Solar Physics Foundation (HSPF)（久洛·拜·佐尔坦太阳观测台，匈牙利太阳物理基金会）
Numerical simulations of large-amplitude oscillations in flux-rope solar prominences
上下文太阳活动的大振幅振荡（LAO）是一种非常壮观但却知之甚少的现象。这些运动具有大于$10 {\mathrm{\, km \,s^{-1}}}$的幅度，并且可以由外部扰动触发，例如，摩顿波或EIT波。目标。我们的目的是分析使用现实的日珥模型的大振幅振荡的性质和触发机制的外部扰动。方法.我们使用具有剪切角和密度对比度两个值的磁通量绳模型对LAO进行了与时间相关的数值模拟。我们利用水平和垂直触发研究了日珥的内部模式。此外，我们使用来自外部的扰动，以了解这种外部干扰如何产生LAO。结果纵向振荡的周期及其随高度的变化与单摆模型吻合得很好。横向振荡的周期随高度保持不变，表明存在一个全局简正模。横向振荡通常具有比纵向振荡更短的周期。结论.纵、横振荡的周期与磁结构的剪切角和日珥密度差的关系很弱。外部扰动扰动的磁通绳激发振荡的两个极化。它们的性质是由纯水平和垂直驱动激发的性质的混合。
