II型射电暴射电增强与太阳高能粒子事件关系的统计

周坤论; 丁留贯; 钱天麒; 朱聪; 王智伟; 封莉

doi:10.7498/aps.69.20200041

摘要

本文基于Learmonth等地面台站和Wind/WAVES, STEREO/SWAVES等卫星射电观测资料, 筛选了第24个太阳活动周2007年1月至2015年12月期间82个米波-十米百米波(meter-decahectometric, M-DH)、十米-百米波(deca-hectometric, DH)II型射电暴事件, 其中39个射电增强事件和43个非射电增强事件. 研究结果显示: 1)射电增强事件的日冕物质抛射(coronal mass ejection, CME)速度、质量、动能和耀斑等级普遍高于无射电增强事件的; 无论有无射电增强, 产生太阳高能粒子(solar energetic particle, SEP)事件的CME速度、质量和动能均明显大于无SEP事件的CME. 2)特征时间分析显示高能粒子起始释放时间普遍早于射电增强开始时间, 由此表明射电增强不是导致高能粒子事件产生的直接原因. 3)无论有无射电增强, SEP事件伴随的II型射电暴开始高度略低于无SEP事件的; 而II型射电暴结束高度, 产生SEP的事件明显高于无SEP的事件; 伴随射电增强的II型射电暴结束高度显著大于无射电增强事件, 即表明有射电增强事件中的激波更强且可持续到更高高度. 4)当快速CME完全扫过另一个先行CME时, CME相互作用更易产生射电增强, 而是否产生SEP无明显差异. 本文结果表明, 射电增强是CME激波与其他CME相互作用而增强的表现, 增强的激波可能增强粒子加速过程而更易产生大的SEP事件, 但射电增强并非产生SEP事件的直接原因.

关键词:

Abstract

In this paper, we investigated 82 type-II radio burst events detected by some ground stations Learmonth, YNAO, and BIRS and spacecraft Wind/WAVES, STEREO/WAVES from January 2007 to December 2015. And we identified 39 events associated with radio enhancement and 43 events without enhancement. We found that: 1) The CME velocity, mass, kinetic energy and flare class with respect to type II radio enhancement events were generally higher than that of no enhancement events, and these properties in the solar energetic particle (SEP) events were significantly higher than that no SEP event, regardless of whether radio enhancement or not. 2) As shown in the characteristic time analysis, the initial release time of SEPs is generally earlier than the start time of radio enhancement, so we can the radio enhancement is only as a signature of the shock enhancement rather than the direct generator of SEP events. 3) Whether radio enhancement or not, the onset height of type IIs associated with SEP event is slightly lower than that of event without SEP. For the absence height, the SEP events are significantly higher than the no-SEP events, and that the absence height of enhancement events are also distinctly higher than that non-enhancement events, which reveals that the enhanced CME shock characterized by enhanced radio burst can keep propagating to more higher or further space. 4) When one fast and wide CME fully sweeps over another slow and narrow preceding CME, CME interaction can more easily generate radio enhancement, but no distinctive difference between SEP events and non-SEP events. So the results of this paper reveal that radio enhancement can be regarded as a manifestation of CME shock becoming strong during interacting with other CME, and the enhanced shock can accelerate the particle to generate large SEP events more easily. However, the type II radio enhancement is not the direct producer or causer that generate large SEP event.

Keywords:

作者及机构信息

1.
南京信息工程大学空间天气研究所, 南京　210044

2.
南京信息工程大学滨江学院, 南京　210044

3.
中国科学院暗物质与空间天文重点实验室, 南京　210008

4.
中国极地研究中心, 上海　200000

通信作者: 丁留贯, dlg@nuist.edu.cn

Authors and contacts

1.
Institute of Space Weather, Nanjing University of Information Science and Technology, Nanjing 210044, China

2.
Binjiang College, Nanjing University of Information Science and Technology, Nanjing 210044, China

3.
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China

4.
China Polar Research Center, Shanghai 200000, China

Corresponding author: Ding Liu-Guan, dlg@nuist.edu.cn

文章全文 : translate this paragraph

参考文献

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施引文献

图 1 (a, c)有射电增强和无射电增强的II型射电暴频谱图; (b, d) CME1, CME2及拟合激波高度-时间变化图

Fig. 1. (a, c) Spectrum diagram of a type II radio burst with and without enhancement; (b, d) the height-time profile of CME1, CME2 and its shock.

下载: 全尺寸图片幻灯片

图 2 CME速度、质量、动能和耀斑统计直方图. 蓝色为有射电增强事件(Group I), 红色为无射电增强事件(Group II)

Fig. 2. Histogram of CME velocity, mass, kinetic energy and flare class. Blue denotes radio enhancement events (Group I), and red denotes no enhancement events (Group II).

下载: 全尺寸图片幻灯片

图 3 SEP事件峰值通量统计直方图

Fig. 3. Statistical histogram of SEP peak intensity.

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图 4 CME速度、质量、动能与SEP事件关联的统计直方图. 蓝色是有SEP事件, 红色是无SEP事件

Fig. 4. Histogram of CME velocity, mass, kinetic energy with SEP/No SEP, and blue denotes the events with SEP, and red denotes the events without SEP.

下载: 全尺寸图片幻灯片

图 5 以SEP事件起始时刻作为参考点0, 各时间点与参考点之差的统计直方图. II型射电暴起始(T1红色)和结束时刻(T2蓝色)、射电增强起始(T3紫色)和结束时刻(T4绿色)、SEP峰值时刻(T5灰色)

Fig. 5. Uses the starting moment of the SEP events as the reference point (0), histogram of the difference between type II radio burst start /stop time(T1/T2), radio enhancement start/stop(T3/T4), SEP stop time(T5) and the reference point respectively.

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图 6 射电增强事件 (a, b) II型射电暴开始、结束高度在不同速度区间内的均值分布; (c, d) II型射电暴开始、结束高度的统计直方图

Fig. 6. For radio enhancement events, (a, b) the bin-average distribution of the type IIs start/stop height in different speed intervals; (c, d) the histogram of the type IIs start/stop height.

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图 7 无射电增强事件 (a), (b) II型射电暴起始、结束高度在不同速度区间内的均值分布; (c), (d)II型射电暴起始、结束高度的统计直方图

Fig. 7. For no radio enhancement events: (a, b) The bin-average distribution of the type IIs start/stop height in different speed intervals; (c, d) the histogram of the type IIs start/stop height.

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图 8 射电增强事件　(a)非增强区域拟合密度模型倍数N1; (b)增强区域拟合密度模型倍数N2; (c) N2与N1差值的统计直方图

Fig. 8. Histogram of N1, N2, N2-N1. N1 and N2 are the multiples of coronal density model used in the fitting of type II radio burst and its enhancement episode respectively.

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图 9 CME1和CME2 速度、角宽、重叠角宽的统计直方图

Fig. 9. Histogram of CME1 and CME2 with speed, angular width and overlap width.

下载: 全尺寸图片幻灯片

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[2]	Kahler S W 2001 J. Geophys. Res. 106 20947 Google Scholar
[3]	Reames D V 1999 Space. Sci. Rev. 90 413 Google Scholar
[4]	Cliver E W, Kahler S W 2004 Astrophys. J. 605 902 Google Scholar
[5]	Gopalswamy N, Xie H, Yashiro S, Akiyama S, Mäkelä P, Usoskin I G 2012 Space. Sci. Rev. 171 23 Google Scholar
[6]	Ding L G, Jiang Y, Li G 2016 Astrophys. J. 818 169 Google Scholar
[7]	Vainio R, Agueda N, Aran A, Lario D 2007 Space Weather. Springer Netherlands. pp 27–37
[8]	Cane H V, von Rosenvinge T T, Cohen C M S, Mewaldt R A 2003 Geophys. Res. Lett. 30 8017 Google Scholar
[9]	Li C, Tang Y H, Dai Y, Fang C, Vial C 2007 Astron. Astrophys. 472 283 Google Scholar
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[12]	Wu S S, Qin G 2018 J. Geophys. Res-Space Phys. 123 76 Google Scholar
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[17]	Gopalswamy N, Yashiro S, Michałek G, Kaiser M L, Howard R A, Reames D V, Leske R, von Rosenvinge T 2002 Astrophys. J. 572 103 Google Scholar
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[19]	Li G, Moore R, Mewaldt R A, Zhao L, Labrador A W 2012 Space. Sci. Rev. 171 141 Google Scholar
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[21]	Gopalswamy N, Aguilar-Rodriguez E, Yashiro S, Nunes S, Kaiser M L, Howard R A 2005 J. Geophys. Res. 110 12 Google Scholar
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[36]	Saito K, Poland A I, Munro R H 1977 Sol. Phys. 55 121 Google Scholar
[37]	Gopalswamy N, S Yashiro 2011 Astrophys. J. 736 17 Google Scholar
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[43]	周坤论, 丁留贯, 王智伟, 封莉 2019 物理学报 68 13 Google Scholar Zhou K L, Ding L G, Wang Z W, Feng L 2019 Acta Phys. Sin. 68 13 Google Scholar
[44]	Bemporad A, Mancuso S 2013 J. Adv. Res. 4 287 Google Scholar
[45]	Sheeley Jr N R, Hakala W N, Wang Y M 2000 J. Geophys. Res. 105 5081 Google Scholar
[46]	Vourlidas A, Wu S T, Wang A H, Subramanian P, Howard R A 2003 J. Adv. Res. 598 1392 Google Scholar
[47]	Cho K S, Lee J, Moon Y J, Dryer M, Bong S C, Kim Y H, Park Y D 2007 Astron. Astrophys. 461 1121 Google Scholar
[48]	Cho K S, Bong S C, Kim Y H, Moon Y J, Dryer M, Shanmugaraju A, Lee J, Park Y D 2008 Astron. Astrophys. 491 873 Google Scholar
[49]	Feng S W, Chen Y, Kong X L, Li G, Song H Q, Feng X S, Ying Liu 2012 Astrophys. J. 753 21 Google Scholar

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II型射电暴射电增强与太阳高能粒子事件关系的统计