Statistical analysis of characteristics of classified type II radio bursts and their associated solar energetic particle events

Zhu Cong; Ding Liu-Guan; Zhou Kun-Lun; Qian Tian-Qi

doi:10.7498/aps.70.20201800

Abstract

In this paper, we investigate 273 type II radio burst events detected by Wind, STEREO spacecraft from January 2010 to March 2018 during the 24th solar cycle. We classify all events as five groups or sub-types according to their starting and ending frequencies, and then analyze the observed characteristics of each group of type II radio bursts and the correlation between the occurrence of solar energetic particle (SEP) events and the associated coronal mass ejection (CME) or type II radio bursts. What we find is as follows. 1) In each group of type II radio burst events, the CME speed (v), width (WD), mass (m), and kinetic energy (E_k) associated with SEP events are generally greater than those with no SEP events, indicating that the generation of SEP events requires a fast and wide energetic CME eruption. 2) Compared with type II radio bursts starting from the DH band, type II radio bursts starting from the metric band have a higher proportion of large SEP events. Multi-band type II radio bursts are more likely to produce SEP events than single-band events, where M-DH-KM type II bursts have the highest proportion of SEP events (73%), and the DH IIs only have the lowest one (19%). 3) In each kind of type II radio bursts, the type IIs with SEP events usually have higher starting frequencies (lower shock forming heights), lower ending frequencies (higher ending heights) and longer durations than those with no SEP events; coronal shock waves that are easy to produce SEP events (especially large SEP events) generally begin to form at a lower height (such as < 3R_s, R_s: solar radius), and are sustained to a much larger height (such as > 30R_s). 4) There exists a strong negative correlation between the duration and the ending frequency of type II radio burst (cc = –0.93). The proportion of SEP events increases with the increase of the duration of type II radio burst, and decreases with the increase of the ending frequency, which largely depends on the CME speed and other properties. The results of this paper further show that the generation of SEP events is greatly related to the sub-types and characteristics of type II radio bursts. The higher the starting frequencies and the lower the ending frequencies of type II radio bursts, such as M-DH-KM type II bursts, of which the CME drives to forming shock waves at a very low height and propagates to a very large height, the longer the duration of the shock, the longer the time it takes to accelerate the particles, and the greater the probability of SEP events (especially large SEP events) is.

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, Chinese Academy of Sciences, Nanjing 210008, China
4.
Guangxi Meteorological Center of Technology and Equipment, Nanning 530022, China

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

Funds: Project supported by the Program of Joint Funds of the National Natural Science Foundation of China (Grant No. U1731105), the Natural Science Foundation of Jiangsu Province, China (Grant No. BK20171456), the Specialized Research Fund for Key Laboratory of Dark Matter and Space Astronomy, Chinese Academy of Sciences, and the Science Research Project of Binjiang College, Nanjing University of Information Science and Technology, China (2020)

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References

[1]	Mclean D J, Labrum N R 1985 Astron. Nachr. 308 182 Google Scholar
[2]	Benz A O 1986 Sol. Phys. 104 99 Google Scholar
[3]	Payne-Scott R, Yabsley D E, Bolton J G 1947 Nature 160 256 Google Scholar
[4]	Wild J P, McCready L L 1950 Aust. J. Chem. 3 387 Google Scholar
[5]	Nelson G J, Melrose D B 1985 Type II Bursts (Cambridge and New York: Cambridge University Press) pp333−359
[6]	Cane H V 1983 Solar Physics (Pasadena: JPL Solar Wind Five) pp703−709
[7]	Gopalswamy N, Thompson B J 2000 J. Atmos. Solar-Terr. Phys. 62 1457 Google Scholar
[8]	Cane H V, Stone R G, Fainberg J, Stewart R T, Steinberg J L, Hoang S 1981 Geophys. Res. Lett. 8 1285 Google Scholar
[9]	Prakash O, Umapathy S, Shanmugaraju A, Vršnak B 2009 Sol. Phys. 258 105 Google Scholar
[10]	Prakash O, Umapathy S, Shanmugaraju A, Pappa Kalaivani P, Vršnak B 2010 Sol. Phys. 266 135 Google Scholar
[11]	Gopalswamy N, Yashiro S, Kaiser M L, Howard R A, Bougeret J L 2001 J. Geophys. Res. Atmos. 106 29219 Google Scholar
[12]	Lara A, Gopalswamy N, Nunes S, Muñoz G, Yashiro S 2003 J. Geophys. Res. 30 8016 Google Scholar
[13]	Reams D V 1995 Rev. Geophys. 33 585 Google Scholar
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[16]	Kahler S W, Vourlidas A 2005 J. Geoghys. Res. 110 A12S01 Google Scholar
[17]	Kahler S W 2001 J. Geophys. Res. 106 20947 Google Scholar
[18]	Kahler S W, Vourlidas A 2014 Astrophys. J. 784 47 Google Scholar
[19]	Desai M, Giacalone J 2016 Rev. Sol. Phys. 13 3 Google Scholar
[20]	Lugaz N, Temmer M, Wang Y M, Farrugia C J 2017 Sol. Phys. 292 64 Google Scholar
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[24]	Zhao M X, Le G M 2020 Res. Astron. Astrophys. 20 037 Google Scholar
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[27]	Gopalswamy N, Aguilar-Rodriguez E, Yashiro S, Nunes S, Kaiser M L, Howard R A 2005 J. Geophys. Res. 110 A12S07 Google Scholar
[28]	Winter L M, Ledbetter K, 2015 Astrophys. J. 809 105 Google Scholar
[29]	陈玉林, 季晶晶, 董丽花, 丁留贯, 李鹏 2015 大气科学学报 38 259 Google Scholar Chen Y L, Ji J J, Dong L H, Ding L G, Li P 2015 Trans. Atmos. Sci. 38 259 Google Scholar
[30]	Marqué C, Posner A, Klein K L 2006 Astrophys. J. 642 1222 Google Scholar
[31]	Kahler S W 2005 Astrophys. J. 628 1014 Google Scholar
[32]	Su W, Cheng X, Ding M D, Sun J Q 2015 Astrophys. J. 804 88 Google Scholar
[33]	王智伟, 丁留贯, 周坤论, 乐贵明 2018 地球 61 3515 Google Scholar Wang Z W, Ding L G, Zhou K L, Le G M 2018 Chin. J. Geophys. 61 3515 Google Scholar
[34]	Ding L G, Wang Z W, Feng L, Li G, Jiang Y 2019 Res. Astron. Astrophys. 19 001 Google Scholar
[35]	Tylka A J, Cohen C M S, Dietrich W F, Krucker S, McGuire R E, Mewaldt R A, Ng C K, Reames D V, Share G H 2003 Proceeding of the 28th International Cosmic Ray Conference Tsukuba, Japan, July 31−August 7, 2003 p3305
[36]	Kim R S, Cho K S, Lee J, Bong S C, Park Y D 2014 J. Geophys. Res. A: Space Phys. 119 9419 Google Scholar
[37]	Ding L G, Cao X X, Wang Z W, Le G M 2016 Res. Astron. Astrophys. 16 8 Google Scholar
[38]	Bemporad A, Manceso S 2013 J. Adv. Res. 4 287 Google Scholar
[39]	周坤论, 丁留贯, 王智伟, 封莉 2019 68 139601 Google Scholar Zhou K L, Ding L G, Wang Z W, Feng L 2019 Acta Phys. Sin. 68 139601 Google Scholar
[40]	Shanmugaraju A, Moon Y J, Dryer M, Umapathy S 2003 Sol. Phys. 217 301 Google Scholar
[41]	周坤论, 丁留贯, 钱天麒, 朱聪, 王智伟, 封莉 2020 69 169601 Google Scholar Zhou K L, Ding L G, Qian T Q, Zhu C, Wang Z W, Feng L 2020 Acta Phys. Sin. 69 169601 Google Scholar

Cited By

图 1 CME速度、角宽、质量和动能统计直方图

Figure 1. Histogram of CME speed (v), angular width (WD), mass (m) and kinetic energy (E_k).

DownLoad: Full-Size Img PowerPoint

图 2 耀斑等级统计直方图

Figure 2. Histogram of solar flare classes.

DownLoad: Full-Size Img PowerPoint

图 3 (a) II型射电暴起始频率分布; (b)−(f) 五类II型射电暴起始频率统计直方图(G1−G5)

Figure 3. (a) Starting frequency distribution of type II radio bursts; (b)−(f) histogram of the starting frequencies of type II radio bursts for five groups (G1−G5).

DownLoad: Full-Size Img PowerPoint

图 4 (a) II型射电暴结束频率分布; (b)−(f) 五类II型射电暴结束频率统计直方图(G1−G5)

Figure 4. (a) Ending frequency distribution of type II radio bursts; (b)−(f) histogram of the ending frequencies of type II radio bursts for five groups (G1−G5).

DownLoad: Full-Size Img PowerPoint

图 5 (a) II型射电暴持续时间分布; (b)−(f) 五类II型射电暴持续时间统计直方图(G1−G5)

Figure 5. (a) Duration distribution of type II radio bursts; (b)−(f) histogram of the durations of type II radio burst for five groups (G1−G5).

DownLoad: Full-Size Img PowerPoint

图 6 (a)−(e) II型射电暴持续时间与结束频率关系; (f), (g) 持续时间和结束频率各区间SEP事件百分比

Figure 6. (a)−(e) Relationship between duration and ending frequency of type II radio bursts; (f), (g) percentage of SEP events in each interval of duration and ending frequency.

DownLoad: Full-Size Img PowerPoint

图 7 II型射电暴起始高度的统计直方图

Figure 7. Histogram of the starting heights of the different group of type II radio bursts.

DownLoad: Full-Size Img PowerPoint

图 8 II型射电暴结束高度的统计直方图

Figure 8. Histogram of the ending heights of the different group of type II radio bursts.

DownLoad: Full-Size Img PowerPoint

图 9 II型射电暴维持高度统计直方图

Figure 9. Histogram of the sustained heights of the type II radio bursts.

DownLoad: Full-Size Img PowerPoint

表 1 II型射电暴伴随SEP事件的统计表

Table 1. SEP events associated with different group of type II radio bursts.

事件类型	G1	G2	G3	G4	G5	All
IIs事件数	107	32	36	38	60	273
无SEP事件数	80	26	20	22	16	164
SEP事件数	27	6	16	16	44	109
SEP事件占比/%	25	19	44	42	73	40
大SEP事件数	13	3	12	13	40	81
大SEP事件占比/%	12	9	33	34	67	30
SEP事件强度均值	0.53	0.02	0.49	4.89	38.74	16.41
SEP事件强度中值	0.01	0.01	0.2	0.24	0.53	0.09
大SEP事件强度均值	1.09	0.04	0.65	6.02	42.62	22.28
大SEP事件强度中值	0.13	0.02	0.33	0.25	0.6	0.34

DownLoad: CSV

表 2 耀斑特征时间统计表

Table 2. Characteristic times of associated solar flares.

类型	T 1/min		T 2/min
类型	均值	中值	均值	中值
G1: M IIs only	14	10	26	19
G2: DH IIs only	38	18	66	33
G3: M-DH IIs	19	16	32	27
G4: DH-KM IIs	35	23	70	52
G5: M-DH-KM IIs	46	22	73	49

DownLoad: CSV

map

[1]	Mclean D J, Labrum N R 1985 Astron. Nachr. 308 182 Google Scholar
[2]	Benz A O 1986 Sol. Phys. 104 99 Google Scholar
[3]	Payne-Scott R, Yabsley D E, Bolton J G 1947 Nature 160 256 Google Scholar
[4]	Wild J P, McCready L L 1950 Aust. J. Chem. 3 387 Google Scholar
[5]	Nelson G J, Melrose D B 1985 Type II Bursts (Cambridge and New York: Cambridge University Press) pp333−359
[6]	Cane H V 1983 Solar Physics (Pasadena: JPL Solar Wind Five) pp703−709
[7]	Gopalswamy N, Thompson B J 2000 J. Atmos. Solar-Terr. Phys. 62 1457 Google Scholar
[8]	Cane H V, Stone R G, Fainberg J, Stewart R T, Steinberg J L, Hoang S 1981 Geophys. Res. Lett. 8 1285 Google Scholar
[9]	Prakash O, Umapathy S, Shanmugaraju A, Vršnak B 2009 Sol. Phys. 258 105 Google Scholar
[10]	Prakash O, Umapathy S, Shanmugaraju A, Pappa Kalaivani P, Vršnak B 2010 Sol. Phys. 266 135 Google Scholar
[11]	Gopalswamy N, Yashiro S, Kaiser M L, Howard R A, Bougeret J L 2001 J. Geophys. Res. Atmos. 106 29219 Google Scholar
[12]	Lara A, Gopalswamy N, Nunes S, Muñoz G, Yashiro S 2003 J. Geophys. Res. 30 8016 Google Scholar
[13]	Reams D V 1995 Rev. Geophys. 33 585 Google Scholar
[14]	Reams D V 1999 Space. Sci. Rev. 90 413 Google Scholar
[15]	Kahler S W 1996 Amer. Inst. Phys. 374 61 Google Scholar
[16]	Kahler S W, Vourlidas A 2005 J. Geoghys. Res. 110 A12S01 Google Scholar
[17]	Kahler S W 2001 J. Geophys. Res. 106 20947 Google Scholar
[18]	Kahler S W, Vourlidas A 2014 Astrophys. J. 784 47 Google Scholar
[19]	Desai M, Giacalone J 2016 Rev. Sol. Phys. 13 3 Google Scholar
[20]	Lugaz N, Temmer M, Wang Y M, Farrugia C J 2017 Sol. Phys. 292 64 Google Scholar
[21]	Le G M, Li C, Zhang X F 2017 Res. Astron. Astrophys. 17 073 Google Scholar
[22]	Le G M, Zhang X F 2017 Res. Astron. Astrophys. 17 123 Google Scholar
[23]	Zhao M X, Le G M, Chi Y T 2018 Res. Astron. Astrophys. 18 074 Google Scholar
[24]	Zhao M X, Le G M 2020 Res. Astron. Astrophys. 20 037 Google Scholar
[25]	Gopalswamy N, Yashiro S, Lara A, Kaiser M L, Thompson B J, Gallagher P T, Howard R A 2003 Goephys. Res. Lett. 30 12 Google Scholar
[26]	Cliver E W, Kahler S W 2004 Astrophys. J. 605 902 Google Scholar
[27]	Gopalswamy N, Aguilar-Rodriguez E, Yashiro S, Nunes S, Kaiser M L, Howard R A 2005 J. Geophys. Res. 110 A12S07 Google Scholar
[28]	Winter L M, Ledbetter K, 2015 Astrophys. J. 809 105 Google Scholar
[29]	陈玉林, 季晶晶, 董丽花, 丁留贯, 李鹏 2015 大气科学学报 38 259 Google Scholar Chen Y L, Ji J J, Dong L H, Ding L G, Li P 2015 Trans. Atmos. Sci. 38 259 Google Scholar
[30]	Marqué C, Posner A, Klein K L 2006 Astrophys. J. 642 1222 Google Scholar
[31]	Kahler S W 2005 Astrophys. J. 628 1014 Google Scholar
[32]	Su W, Cheng X, Ding M D, Sun J Q 2015 Astrophys. J. 804 88 Google Scholar
[33]	王智伟, 丁留贯, 周坤论, 乐贵明 2018 地球 61 3515 Google Scholar Wang Z W, Ding L G, Zhou K L, Le G M 2018 Chin. J. Geophys. 61 3515 Google Scholar
[34]	Ding L G, Wang Z W, Feng L, Li G, Jiang Y 2019 Res. Astron. Astrophys. 19 001 Google Scholar
[35]	Tylka A J, Cohen C M S, Dietrich W F, Krucker S, McGuire R E, Mewaldt R A, Ng C K, Reames D V, Share G H 2003 Proceeding of the 28th International Cosmic Ray Conference Tsukuba, Japan, July 31−August 7, 2003 p3305
[36]	Kim R S, Cho K S, Lee J, Bong S C, Park Y D 2014 J. Geophys. Res. A: Space Phys. 119 9419 Google Scholar
[37]	Ding L G, Cao X X, Wang Z W, Le G M 2016 Res. Astron. Astrophys. 16 8 Google Scholar
[38]	Bemporad A, Manceso S 2013 J. Adv. Res. 4 287 Google Scholar
[39]	周坤论, 丁留贯, 王智伟, 封莉 2019 68 139601 Google Scholar Zhou K L, Ding L G, Wang Z W, Feng L 2019 Acta Phys. Sin. 68 139601 Google Scholar
[40]	Shanmugaraju A, Moon Y J, Dryer M, Umapathy S 2003 Sol. Phys. 217 301 Google Scholar
[41]	周坤论, 丁留贯, 钱天麒, 朱聪, 王智伟, 封莉 2020 69 169601 Google Scholar Zhou K L, Ding L G, Qian T Q, Zhu C, Wang Z W, Feng L 2020 Acta Phys. Sin. 69 169601 Google Scholar

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