太阳高能粒子观测特征经向分布统计

钱天麒; 丁留贯; 周坤论; 王智伟; 朱聪

doi:10.11728/cjss2021.03.355

太阳高能粒子观测特征经向分布统计

doi: 10.11728/cjss2021.03.355 cstr: 32142.14.cjss2021.03.355

钱天麒¹,
丁留贯^1,2,3,
周坤论¹,
王智伟^1,4,
朱聪¹

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 200136

基金项目:

国家自然科学基金天文联合基金项目（U1731105），江苏省基础研究计划面上项目（BK20171456），中国科学院暗物质与空间天文重点实验室开放课题和国家重点研发计划项目（2018YFC1407304，2018YFF01013706）共同资助

详细信息

作者简介:

丁留贯,E-mail:dlg@nuist.edu.cn

中图分类号: P353
计量
- 文章访问数: 942
- HTML全文浏览量: 187
- PDF下载量: 81
- 被引次数:
  0(来源:Crossref)
  
  0(来源:其他)
出版历程
- 收稿日期: 2020-05-19
- 修回日期: 2021-02-07
- 刊出日期: 2021-05-15

Statistical Research on the Longitudinal Distribution of Detected Properties of Solar Energetic Particles

1. Institute of Space Weather, Nanjing University of Information Science and Technology, Nanjing 210044;
2. Binjiang College, Nanjing University of Information Science and Technology, Nanjing 210044;
3. Key Laboratory of Dark Matter and Space Astronomy, Chinese Academy of Sciences, Nanjing 210008;
4. China Polar Research Center, Shanghai 200136

摘要

摘要: 基于多卫星联合观测数据，筛选了2006年12月至2017年10月期间122个太阳高能粒子（SEP）事件及其伴随的日冕物质抛射（CME），分析了SEP事件属性随相对经度的变化、与CME属性之间相关性的经向分布以及与Fe/O比值的关联.研究结果显示：低Fe/O类事件的峰值通量I_p通常更高，伴随CME更大，但通量上升速度较慢，且其D_u（持续时间）和I_p与CME速度呈现更强的相关性；SEP特征时间T_O（CME爆发至SEP事件爆发）与T_R（SEP事件爆发至半峰值）随相对经度增加而增大，D_u与I_p随相对经度增加而减小，通量上升斜率K在±90°范围内自东向西递减；SEP事件属性与伴随CME属性的相关性随相对经度的改变有明显变化，在磁连接好的位置，T_O与CME速度等属性呈现负相关，T_R与CME速度等属性呈现正相关，D_u，I_p与CME速度之间的相关性更强.研究结果进一步表明，SEP事件观测属性既与CME参数相关，同时又具有很强的经度依赖性，在磁连接越好的位置卫星观测到的SEP事件强度越高，SEP观测参数受CME的影响越大，这对大型SEP事件的预报很有意义.此外，高Fe/O类SEP事件与CME相关性的减弱暗示了耀斑加速、种子粒子源等因素的影响.
- 太阳高能粒子 /
- 日冕物质抛射 /
- 相对经度 /
- 铁氧比
Abstract: Using the observations from multi-points spacecraft, e.g., SOHO and STEREO, 122 SEP events and associated CMEs during the 24th solar cycle from December 2006 to October 2017 are selected. The longitudinal distributions of SEP characteristics and their relationship with CMEs properties are analyzed, as well as the relation with the event-integrated Fe/O ratio. Results are shown as follows: Large SEP events usually have a lower Fe/O ratio, while those events with high Fe/O have lower CME velocity, mass and kinetic energy, but have faster flux rising speed. The duration D_u and peak flux I_p of SEP correlate well with the associated CME velocity positively (correlation coefficient, CC: 0.50 and 0.57). Comparing to the events with a high Fe/O ratio, the events with low Fe/O obviously have much higher correlation coefficients for D_u and I_p with CME. The characteristic time T_O and T_R of SEPs generally increases with the raising of relative longitude, while D_u and I_p decrease distinctly with the raising of relative longitude. And the slope K of the SEPs flux enhancing in the onset phase seems to decrease from the east (-90°) to west (90°) relative to the source region. T_O shows a negative correlation with CME velocity, mass and kinetic energy in the magnetic well-connected points, while there is no distinct correlation in other poor-connected points. Meanwhile, T_R has a positive correlation with CME only in the relative longitude range of [-30°, +30°]. D_u and I_p have a stronger correlation with CME velocity in the well-connected condition (CC: 0.60 and 0.75 respectively) than others (0.46 and 0.56). The conclusion reveals that the detection of SEP event and its time profile evolution is not only affected by the associated CME, but also controlled by the relative longitude between the magnetic foot point and the solar eruption source, and for the well-connected points, the detectable SEP event has more high intensity and good positive correlation with its associated CME, which is very important for the space weather prediction of SEP events, especially large or extremely large SEP events. Moreover, the SEP event with a high Fe/O ratio seems to become weaker among the relationship with CME, which implies that some facts such as flare acceleration, seed population, and so on, will play important roles during the generation of gradual SEP events associated with CME-driven shock.
- Solar Energetic Particle /
- Coronal Mass Ejection /
- Relative longitude /
- Fe/O ratio

HTML全文

参考文献(31)

[1]	KAHLER S W, REAMES D V, SHEELEY N R. Coronal mass ejections associated with impulsive solar energetic particle events[J]. Astrophys. J., 2001, 562(1):558-565
[2]	CANE H V, MCGUIRE R E, VON ROSENVINGE T T. Two classes of solar energetic particle events associated with impulsive and long-duration soft X-ray flares[J]. Astrophys. J., 1986, 301(1):448-459
[3]	REAMES D V. Particle acceleration at the sun and in the heliosphere[J]. Space Sci. Rev., 1999, 90(3/4):413-491
[4]	CLIVER E W, SVALGAARD L. The 1859 solar-terrestrial disturbance and the current limits of extreme space weather activity[J]. Sol. Phys., 2004, 224(1/2):407-422
[5]	KLEIN K L, KRUCKER S, LOINTIER G, et al. Open magnetic flux tubes in the corona and the transport of solar energetic particles[J]. Astron. Astrophys., 2008, 486(2):589-596
[6]	CANE H V, REAMES D V, VON ROSENVINGE T T. The role of interplanetary shocks in the longitude distribution of solar energetic particles[J]. J. Geophys. Res., 1988, 93(A9):9555-9567
[7]	GOPALSWAMY N. Intensity variation of large solar energetic particle events associated with coronal mass ejections[J]. J. Geophys. Res., 2004, 109(A12):A12105
[8]	DING L G, JIANG Y, ZHAO L L, et al. The “twin-CME” scenario and large solar energetic particle events in solar cycle 23[J]. Astrophys. J., 2013, 763(30):17
[9]	TYLKA A J, COHEN C M S, DIETRICH W F, et al. Shock geometry, seed populations, and the origin of variable elemental composition at high energies in large gradual solar particle events[J]. Astrophys. J., 2005, 625:474-495
[10]	SOKOLOV I V, ROUSSEV I I, FISK L A, et al. Diffusive shock acceleration theory revisited[J]. Astrophys. J. Lett., 2006, 642:81-84
[11]	KAHLER S W. Energetic particle acceleration by coronal mass ejections[J]. Adv. Space. Res., 2003, 32(12):2587-2596
[12]	DING L G, CAO X X, WANG Z W, et al. Large solar energetic particle event that occurred on 2012 March 7 and its VDA analysis[J]. Res. Astron. Astrophys., 2016, 16(8):122
[13]	RUFFOLO D, TOOPRAKAI P, RUJIWARODOM M, et al. Relativistic solar protons on 1989 October 22: injection and transport along both legs of a closed interplanetary magnetic loop[J]. Astrophys. J., 2016, 639(2):1186-1205
[14]	RICHARDSON I G, CANE H V, VON ROSENVINGE T T. Prompt arrival of solar energetic particles from far eastern events: the role of large-scale interplanetary magnetic field structure[J]. J. Geophys. Res., 1991, 96(A5):7853-7860
[15]	LARIO D, RAOUAFI N E, KWON R Y, et al. The solar energetic particle event on 2013 April 11: an investigation of its solar origin and longitudinal spread[J]. Astrophys. J., 2014, 797(8):16
[16]	LARIO D, KWON R-Y, RICHARDSON I G, et al. The solar energetic particle event of 2010 August 14: connectivity with the solar source inferred from multiple spacecraft observations and modeling[J]. Astrophys. J., 2017, 838(1):24
[17]	LARIO D, ARAN A, GOMEZ HERRERO R, et al. Longitudinal and radial dependence of solar energetic particle peak intensities: STEREO, ACE, SOHO, GOES, and MESSENGER observations[J]. Astrophys. J., 2013, 767(41):18
[18]	HE H Q, WAN W. On the east-west longitudinally asymmetric distribution of solar proton events[J]. Mon. Not. R. Astron. Soc., 2016, 2255.DOI: 10.1093/mnras/stw2255
[19]	KAHLER S W. Characteristic times of gradual solar energetic particle events and their dependence on associated coronal mass ejection properties[J]. Astrophys. J., 2005, 628:1014-1022
[20]	JIAN Yi, LAI Min, DING Liuguan. Statistical study on the ascending time of solar energetic particle events (in Chinese)[J]. Chin. J. Space. Sci., 2014, 34(6):785-793(简昳, 赖敏, 丁留贯. 太阳高能粒子事件上升事件统计研究[J]. 空间科学学报, 2014, 34(6):785-793)
[21]	RICHARDSON I G, VON ROSENVINGE T T, CANE H V, et al. >25MeV proton events observed by the high energy telescopes on the STEREO A and B spacecraft and/or at Earth during the first seven years of the STEREO mission[J]. Sol. Phys., 2014, 289(8):3059-3107
[22]	CANE H V, MEWALDT R A, COHEN C M S, et al. Role of flares and shocks in determining solar energetic particle abundances[J]. J. Geophys. Res., 2006, 111(A06S90).DOI: 10.1029/2005JA011071
[23]	DING L G, LI G, LE G M, et al. Seed population in large solar energetic particle events and the twin-CME scenario[J]. Astrophys. J., 2015, 812(2):171
[24]	WANG Zhiwei, DING Liuguan, ZHOU Kunlun, et al. On the relationship between large SEP event and twin-CME with the observations from multiple-vantage spacecraft (in Chinese)[J]. Chin. J. Geophy., 2018, 61(9):3515-3525(王智伟, 丁留贯, 周坤论, 等. 基于多视角观测的SEP事件与twin-CME关系研究[J]. 地球物理学报, 2018, 61(9):3515-3525)
[25]	DING L G, WANG Z W, FENG L, et al. Is the enhancement of type II radio bursts during CME interactions related to the associated solar energetic particle event[J]. Res. Astron. Astrophys., 2019, 19(1):5
[26]	LI C, TANG Y H, DAI Y, et al. The acceleration characteristics of solar energetic particles in the 2000 July 14 event[J]. Astron. Astrophys., 2007, 461(3):1115-1119
[27]	LI C, TANG Y H, DAI Y, et al. Flare magnetic reconnection and relativistic particles in the 2003 October 28 event[J]. Astron. Astrophys., 2007, 472(1):283-286
[28]	ROUILLARD A P, ODSTŘCIL D, SHEELEY N R, et al. Interpreting their properties of solar energetic particle events by using combined imaging and modeling of interplanetary shocks[J]. Astrophys. J., 2011, 735(1):7
[29]	ROUILLARD A P, SHEELEY N R, TYLKA A, et al. The longitudinal properties of a solar energetic particle event investigated using modern solar imaging[J]. Astrophys. J., 2012, 752(1):44
[30]	KAHLER S W, VOURLIDAS A. A comparison of the intensities and energies of gradual solar energetic particle with the dynamical properties of associated coronal mass ejections[J]. Astrophys. J., 2013, 769(2):143
[31]	KAHLER S W, VOURLIDAS A. Do interacting coronal mass ejections play a role in solar energetic particle events[J]. Astrophys. J., 2014, 784(1):47