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The Polar Surge and Macrospicule Obsered by EIT/SOHO
Kwon, Ryun Young,Jang, Minhwan 경희대학교 자연과학종합연구원 2003 자연과학논문집 Vol.9 No.1
SOHO 위성의 EIT를 이용한 λ304Å의 태양 Full Disk Image에서 Coronal Hole에서 특징적으로 발생하는 Polar Surge와 Macrospicule을 분석하여 이전에 보고된 결과들과 비교해 본다. 이들은 태양의 Coronal Hole에서만 제한적으로 나타나며 단일한 선으로 나타나지 않고 군을 이루어 나타나는 모습을 보여준다. 그리고 발생한 위치에서 반복적으로 다시 관측이 되는 경향을 보인다. 이전에 보고되어진 것들보다 월등히 크기가 큰 현상들과, 반면 지속시간이 짧은 Polar Surge와 Macrospicule을 발견하였다. An analysis of the polar surge and macrospicule is reported. The images of the polar surge and macrospicule were compared with previous works using sequence of EIT λ304Å images in the solar south coronal hole. The macrospicule and polar surge are limited to the solar coronal hole and are consisted of one or more overlapping mount-like features. They tend to re-occur at the same place. It is found out that our results showing distinguishing characters such as a larger length and shorter lifetime are not coincided with the works of previous researchers.
조경석,권륜영,김록순,Cho, Kyungsuk,Gopalswamy, Nat,Kwon, Ryunyoung,Kim, Roksoon,Yashiro, Seiji 한국천문학회 2012 天文學會報 Vol.37 No.2
We examine the relationship between a type II radio burst that started from an unusually high frequency of 425 MHz (fundamental component) and an associated white-light coronal mass ejection on 2011 February 13. The radio burst had a drift rate of 2.5 MHz/sec, indicating a relatively high shock speed. From SDO AIA observations we find that a loop-like erupting front sweeps across high density coronal loops near the start time of the burst (17:34:15 UT). We find fragmented structures of the type II burst, which indicates the signature of the shock propagating through the multiple loops. The deduced distance of shock formation (0.06 Rs) from flare center and speed of the shock (1100 km $s^{-1}$) using the measured density from AIA/SDO observations are comparable to the height (0.05 Rs, from the solar surface) and speed (700 km $s^{-1}$) of the CME leading edge observed by STEREO/EUVI. We conclude that the type II burst could be onset even in the low corona (41 Mm or 0.06 Rs, above the solar surface) if a fast CME shock passes through the high density loops.