Statistical analysis of the relationship between type II radio enhancement and solar energetic particle event

Zhou Kun-Lun; Ding Liu-Guan; Qian Tian-Qi; Zhu Cong; Wang Zhi-Wei; Feng Li

doi:10.7498/aps.69.20200041

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:

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

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References

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Cited By

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

Figure 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.

DownLoad: Full-Size Img PowerPoint

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)

Figure 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).

DownLoad: Full-Size Img PowerPoint

图 3 SEP事件峰值通量统计直方图

Figure 3. Statistical histogram of SEP peak intensity.

DownLoad: Full-Size Img PowerPoint

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

Figure 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.

DownLoad: Full-Size Img PowerPoint

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)

Figure 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.

DownLoad: Full-Size Img PowerPoint

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

Figure 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.

DownLoad: Full-Size Img PowerPoint

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

Figure 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.

DownLoad: Full-Size Img PowerPoint

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

Figure 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.

DownLoad: Full-Size Img PowerPoint

图 9 CME1和CME2 速度、角宽、重叠角宽的统计直方图

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

DownLoad: Full-Size Img PowerPoint

[1]	Vršnak B, Cliver E W 2008 Sol. Phys. 253 215 Google Scholar
[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
[10]	Le G M, Zhang X F 2017 Res. Astron. Astrophys. 17 123 Google Scholar
[11]	Le G M, Li C, Zhang X F 2017 Res. Astron. Astrophys. 17 73 Google Scholar
[12]	Wu S S, Qin G 2018 J. Geophys. Res-Space Phys. 123 76 Google Scholar
[13]	Zhao M X, Le G M, Chi Y T 2018 Res. Astron. Astrophys. 18 74 Google Scholar
[14]	Zhao M X, Le G M 2020 Res. Astron. Astrophys. 20 37 Google Scholar
[15]	Mason G M, Mazur J E, Dwyer J R 1999 Astrophys. J. 525 133 Google Scholar
[16]	Mason G M, Dwyer J R, Mazur J E 2000 Astrophys. J. 545 157 Google Scholar
[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
[18]	Gopalswamy N, Yashiro S, Krucker S, Stenborg G, Howard R A 2004 J. Geophys. Res-Space. 109 12105 Google Scholar
[19]	Li G, Moore R, Mewaldt R A, Zhao L, Labrador A W 2012 Space. Sci. Rev. 171 141 Google Scholar
[20]	Shen C L, Wang Y M, Ye P Z, Zhao X P, Gui B, Wang S 2007 Astrophys. J. 670 849 Google Scholar
[21]	Gopalswamy N, Aguilar-Rodriguez E, Yashiro S, Nunes S, Kaiser M L, Howard R A 2005 J. Geophys. Res. 110 12 Google Scholar
[22]	Winter L M, Ledbetter K 2015 Astrophys. J. 809 105 Google Scholar
[23]	Gopalswamy N, Yashiro S, Kaiser M L, Howard R A, Bougeret J L 2001 Astrophys. J. 548 91 Google Scholar
[24]	Ding L G, Li G, Jiang Y, Le G M, Shen C L, Wang Y M, Chen Y, Xu F, Gu B, Zhang Y N 2014 Astrophys. J. 793 35 Google Scholar
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[29]	von Rosenvinge T T, Reames D V, Baker R, Hawk J, Nolan J T, Ryan L, Shuman S, Wortman K A, Mewaldt R A, Cummings A C, Cook W R, Labrador A W, Leske R A, Wiedenbeck M E 2008 Space. Sci. Rev. 136 391 Google Scholar
[30]	王智伟, 丁留贯, 周坤论, 乐贵明 2018 地球物理学报 61 3515 Google Scholar Wang Z W, Ding L G, Zhou K L, Le G M 2018 Chin. J. Geophys. 61 3515 Google Scholar
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[32]	Kim R S, Cho K S, Lee J, Bong S C, Park Y D 2014 J. Geophys. Res-Space. 119 9419 Google Scholar
[33]	乐贵明, 唐玉华, 韩延本 2007 科学通报 52 2461 Google Scholar Le G M, Tang Y H, Han Y B 2007 Chin. Sci. Bull. 52 2461 Google Scholar
[34]	Newkirk G Jr 1961 Astrophys. J. 133 983 Google Scholar
[35]	Vršnak B, Magdalenić J, Zlobec P 2004 Astron. Astrophys. 413 753 Google Scholar
[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
[38]	Mäkelä P, Gopalswamy N, Akiyama S, Xie H, Yashiro S 2015 Astrophys. J. 806 13 Google Scholar
[39]	Kocharov L, Pohjolainen S, Mishev A, Reiner M J, Lee J, Laitinen T, Didkovsky L V, Pizzo V J, Kim R, Klassen A, Karlicky M, Cho K S, Gary D E, Usoskin I, Valtonen E, Vainio R 2017 Astrophys. J. 839 79 Google Scholar
[40]	Temmer M, Vršnak B, Rollett T, Bein B, Koning D, Liu Y, Bosman E, Davies J A, Most C, Zic T, Veronig A M, Bothmer V, Harrison R, Nitta N, Bisi M, Flor O, Eastwood J, Odstrcil D, Forsyth R 2012 Astrophys. J. 749 57 Google Scholar
[41]	Ding L G, Jiang Y, Zhao L L, Li G 2013 Astrophys. J. 763 30 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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