Ultraviolet Spectroscopic Study on the Fine Structures in the Solar Polar Hole
ZHANG Min1, 2, WANG Dong1, LIU Guo-hong1
1. School of Mathematics and Physics, Anhui University of Architecture, Heifei 230601, China 2. Key Laboratory of Geospace Environment, Chinese Academy of Sciences, School of Earth and Space Science, University of Science and Technology of China, Heifei 230026, China
Abstract：Fine structures in the south solar polar coronal hole were observed by N Ⅳ line of SOHO/SUMER spectrograph. The scales of the fine structures range spatially range from 1 arcsec to several arcsecs, temporally from 1 min to several minutes, and parts of them are in strip shape along the slit direction. The line-of-sight velocity of them is up to tens of km·s-1 with red and blue shift intercrossed occasionally, which appear periodically as long as 100 minutes in some regions. Part of the fine structures can be clearly observed at the Ne ⅤⅢ line with higher formation temperature in the same spectral window. The time and location of some fine structures with high velocity in the Ne ⅤⅢ spectrum are almost the same as that in N Ⅳ spectrum, but they are extended and diffused in the Ne ⅤⅢ spectrum. Some fine structures have non-Gaussian profiles with the line-of-sight Doppler velocities up to 150 km·s-1 in the N Ⅳ blue/red wings, which is similar with the explosive events in the transition region. In the past, explosive events are small-scale dynamic phenomena often observed in the quiet-sun (QS) region, while their properties in coronal holes (CHs) remain unclear. Here, we find the EE-like events with strong dynamics in the south solar polar coronal hole by N Ⅳ line of SOHO/SUMER spectrograph.
章 敏1,2，王 东1，刘果红1 . 太阳极区冕洞内小尺度结构的紫外光谱研究 [J]. 光谱学与光谱分析, 2014, 34(07): 1890-1893.
ZHANG Min1, 2, WANG Dong1, LIU Guo-hong1 . Ultraviolet Spectroscopic Study on the Fine Structures in the Solar Polar Hole . SPECTROSCOPY AND SPECTRAL ANALYSIS, 2014, 34(07): 1890-1893.
[1] LIN Yuan-zhang(林元章), Introduction of Solar Physics(太阳物理导论). Beijing：Science Press(北京：科学出版社)，2000. [2] Innes D E, Inhester B, Axford W I, et al. Nature, 1997, 386. [3] Teriaca L, Banerjee D, Falchi A, et al.Astronomy & Astrophysics, 2004, 427: 1065. [4] Zhang M, Xia L D, Tian H, et al. Astronomy & Astrophysics, 2010, 520: 37. [5] ZHANG Min, XIA Li-dong, HUANG Zheng-hua(章 敏，夏利东，黄正化). Progress in Astronomy(天文学进展)，2010，28(3)：229. [6] Wilhelm K, Curdt W, Marsch E, et al. Sol. Phys., 1995, 162: 189. [7] Delaboudiniere J P, Artzner G E, Brunaud J, et al. Sol. Phys., 1995, 162: 291. [8] Charbonneau, P. The Astrophysical Journal Suppl., 1995 101: 309. [9] Dammasch I E, Wilhelm K, Curdt W, et al. Astronomy & Astrophysics, 1999, 346: 285. [10] Xia L D, Marsch E, Wilhelm K. Astronomy & Astrophysics, 2004, 424: 1025. [11] Curdt W，Tian H, Kamio S. Sol. Phys., 2012, 280: 2. [12] Tian H, Teriaca L, Curdt W, et al. The Astrophysical Journal, 2009, 703: 152. [13] Xia L D, Popescu M D, Doyle J G, et al. Astronomy & Astrophysics, 2005, 438: 1115. [14] Patsourakos S, Vial J C, Gabriel A H, et al. The Astrophysical Journal, 1999, 522: 540. [15] Chae J, Wang H, Lee C Y, et al. The Astrophysical Journal, 1998, 504: L123.
