Intensity variations of the postnoon auroral bright spots observed at Zhongshan Station, Antarctica on August 8, 1999
Intensity variations of the postnoon auroral bright spots observed at Zhongshan Station, Antarctica on August 8, 1999
摘要
In this paper we use the high speed multi channel meridian scanning photometer data and all sky TV camera images to analyze the intensity variations of the postnoon auroral bright sports of 557.7 nm and 630.0 nm emissions. Several results can be obtained from this paper. (1) Bright spots are rather transient features lasting typically for only a few minutes. (2) The intensity of the postnoon bright spots of 557.7 nm emissions can surpass 11 kR. The occurrence of the bright spots seems rather frequent. (3) The ratios of I(427.8)/I(630.0) and I(427.8)/I(557.7) during the bright spots occurring time show a positive peak and negative peak respectively. It qualitatively indicates that the average precipitating electron energies along the meridianal scan above Zhongshan Station increased as the bright spot appeared. And the intensification of the spot mainly was caused by the increasing of high energy (3 10 keV) flux. (4) Usually the bright spots are accompanied with the magnetic pulsation and the occurrence of multi band arcs.
In this paper we use the high speed multi channel meridian scanning photometer data and all sky TV camera images to analyze the intensity variations of the postnoon auroral bright sports of 557.7 nm and 630.0 nm emissions. Several results can be obtained from this paper. (1) Bright spots are rather transient features lasting typically for only a few minutes. (2) The intensity of the postnoon bright spots of 557.7 nm emissions can surpass 11 kR. The occurrence of the bright spots seems rather frequent. (3) The ratios of I(427.8)/I(630.0) and I(427.8)/I(557.7) during the bright spots occurring time show a positive peak and negative peak respectively. It qualitatively indicates that the average precipitating electron energies along the meridianal scan above Zhongshan Station increased as the bright spot appeared. And the intensification of the spot mainly was caused by the increasing of high energy (3 10 keV) flux. (4) Usually the bright spots are accompanied with the magnetic pulsation and the occurrence of multi band arcs.
基金
ThisprojectwassupportedbytheNationalNaturalScienceFounda tionofChina (No .40 0 44 0 1 3 ) .
参考文献10
-
1Eastman TE,Hones EW,Bame SJ.Asbridge JR (1976): The magnetospheric boundary layer, site of plasma,mimentum, and energy transfer from the magnetosheath into the magnetosphere[].Geophysical Research Letters.
-
2Lundin R.Dubinin E (1984): Solar wind energy transfer regions inside the dayside magnetopause, I, Evidence for magnetosheath plasma penetration[].Planetary and Space Science.
-
3Lui ATY,Venkatesan D,Rostoker G,Murphree C,Anger D,Cogger L.Potemra TA (1987): Dayside auroral intensifications during an auroral substorm[].Geophysical Research Letters.
-
4Bruning K,Block LP,Marklund GT.Eliasson L (1990): Viking observations above a postnoon aurora[].Journal of Geophysical Research.
-
5Wei CO.Lee LC (1993): Coupling of magnetopause boundary layer to the polar ionosphere[].Journal of Geophysical Research.
-
6Rostoker GA,Jackel B.Arnoldy RL (1992): The relationship of periodic structures in auroral luminosity in the afternoon sector to ULF pulsations[].Geophysical Research Letters.
-
7Newell PT,Kevin ML,Ching-I.Meng (1996): A large survey of electron acceleration events[].Journal of Geophysical Research.
-
8Cowley SWH,Southwood DJ.Saunders MA ( 1983 ): Interpretation of magnetic field perturbations in the earth’s magnetopause boundary layer[].Planetary and Space Science.
-
9Egeland A,Burke WJ.Maynard NC (1994): Ground and satellite observations of postdawn aurorae near the time of a sudden storm commencement[].Journal of Geophysical Research.
-
10Pu ZY.Kivelson MG (1983): Kelvin-Helmholtz instability at the magnetopause: Solutions for compressible plasma[].Journal of Geophysical Research.
-
1胡红桥,刘瑞源,杨惠根.The auroral occurrence over Zhongshan Station, Antarctica[J].Chinese Journal of Polar Science,1999,10(2):101-109. 被引量：1
-
2Liu Li-gang 1, Ai Yong 1, Liu Rui-yuan 2, Yang Hui-gen 2 1. School of Electronic Information, Wuhan University, Wuhan 430072, Hubei, China,2. Polar Research Institute of China, Shanghai 200129, China.Locating the Polar Cap Boundary of Postnoon Sector from Observations of 630.0 nm Auroral Emission at Zhongshan Station[J].Wuhan University Journal of Natural Sciences,2002,7(1):59-64.
-
3Jiang Xiaojun 1,2 1 Beijing Astronomical Observatory, The Chinese Academy of Sciences, Beijing 100012, China Email: xjjiang @ class1. bao. ac. cn 2 National Astronomical Observatories, The Chinese Academy of Sciences.The 3-channel High-Speed Photometer at Beijing Astronomical Observatory[J].天文研究与技术,1999(S1):68-71. 被引量：1
-
4曹冲.Pulsating aurora - a review[J].Chinese Journal of Polar Science,1995,6(1):39-50.
-
5徐文耀,魏自刚,张北辰,胡红桥,刘瑞源.Determination of apparent bulk velocity of auroral images[J].Chinese Journal of Polar Science,1999,10(2):89-94.
-
6Yang, YG,Liu, RY,Sato, NS.Intensity correction in all-sky auroral image projection transform[J].Chinese Science Bulletin,1997,42(8):700-703. 被引量：5
-
7Ai Yong1, Wang Jing-fang1, Liu Rut-yuan2, Yang Hut-gen 2, Sato Natsuo3 1. College of Electronic information, Wuhan University, Wuhan 4 30072, China 2. Polar Research institute of China, Shanghai 200129, China 3. National Institute of Polar Research, Tokyo, Japan 173.Analysis of Characteristic of Aurora Substorm Observed at Antarctic Zhongshan Station[J].Wuhan University Journal of Natural Sciences,2000,5(3):312-316.
-
8LI Ti-pei (Institute of High Enerpy Physics, The Chinese Academy of Sciences, Beijing 100039).IMAGING IN HIGH ENERGY ASTRONOMY[J].空间科学学报,1998,18(S1):12-20.
-
9Chun-Guang Zhang,Li-Cai Deng,Da-Run Xiong.On the effect of turbulent anisotropy on pulsation stability of stars[J].Research in Astronomy and Astrophysics,2017,17(3):77-86.
-
10De＇er Zhang,Youye Liang.A Long Lasting and Extensive Drought Event over China in 1876-1878[J].Advances in Climate Change Research,2010,1(2):91-99. 被引量：2
