缓变型太阳高能粒子事件特征时间及其经向分布

丁留贯; 曹鑫鑫; 王智伟; 顾斌

doi:10.11728/cjss2018.03.296

缓变型太阳高能粒子事件特征时间及其经向分布

doi: 10.11728/cjss2018.03.296

1 南京信息工程大学空间天气研究所南京 210044;
2 南京信息工程大学物理与光电工程学院南京 210044

基金项目:

国家自然科学基金项目（U1731105，41304150），江苏省基础研究计划面上项目（BK20171456）和江苏省教育厅"青蓝工程"人才项目共同资助

详细信息

作者简介:
丁留贯,E-mail:dlg@nuist.edu.cn

中图分类号: P352
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- 被引次数: 0
出版历程
- 收稿日期: 2017-04-21
- 修回日期: 2018-02-13
- 刊出日期: 2018-05-15

Characteristic Times and Longitudinal Distributions of Gradual Solar Energetic Particle Events

1 Institute of Space Weather, Nanjing University of Information Science and Technology, Nanjing 210044;
2 School of Physics and Optoelectronic Engineering, Nanjing University of Information Science and Technology, Nanjing 210044

摘要

摘要: 利用SOHO，STEREO高能粒子观测数据，对2011-2014年30个通量短时间内显著增强的缓变型太阳高能粒子（SEP）事件的两个特征时间（局地爆发时间，起始释放时间）及其经向分布进行统计分析.研究结果显示，多颗卫星同时观测到的SEP事件伴随的日冕物质抛射（CME）角宽明显较一般事件大，且基本都为Halo CME；不同卫星观测到的粒子通量局地增强时间差与卫星位置经度差明显线性正相关且东西不对称；局地爆发时间和起始释放时间相对于耀斑时间的延迟与卫星相对经度正相关；卫星所有能量通道的两个特征时间极差与卫星相对经度呈现较好的正相关，这表明不同能量SEP释放的时间跨度具有明显经度差异；高低能释放时间差与CME速度正相关.这些结论表明，SEP事件的两个特征时间具有明显的经向依赖性，并都与CME速度相关.
- 太阳高能粒子事件 /
- 特征时间 /
- 经向分布 /
- 日冕物质抛射
Abstract: The two characteristic times (onset time t_ob and release time t_sr) and their longitudinal distribution of 30 gradual Solar Energetic Particle (SEP) events from 2011 to 2014, which particle flux increase remarkably in a short time, are analyzed. The results show that the SEP events observed by multi-spacecraft are usually associated with the wider halo Coronal Mass Ejection (CME) than those of general SEP events. The onset time difference of energetic particles observed by two spacecraft presents a good linear correlation with the longitude difference of two spacecraft, and east-west hemispheric asymmetry. The time intervals between the onset and release time and the flare onset are positively correlated with the relative longitude of the detector to the active region. The range of onset time or release time (t_slow-t_fast) in different energy channels for one SEP event shows a good positive correlation with the relative longitude of spacecraft, and release time ranges in different energy channels have a distinct longitudinal distribution. The release time interval between high and low energy channel has a positive correlation with CME speed. Therefore, the two characteristic times, in-situ onset time and solar particle release time near the sun, have obvious longitudinal distributions, and a strong correlation with the associated CME.
- Solar Energetic Particle (SEP) events /
- Characteristic time /
- Longitudinal distribution /
- Coronal Mass Ejection (CME)

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参考文献(23)

[1]	KAHLER S W. Coronal mass ejections and solar energetic particle events[J]. AIP Conf. Proc., 1996, 374(1):61-77
[2]	REAMES D V. Solar energetic-particle release times in historic ground-level events[J]. Astrophys. J., 2009, 706(1):844-850
[3]	REAMES D V. Solar release times of energetic particles in ground-level events[J]. Astrophys. J., 2009, 693(1):812-821
[4]	EYLES C J, HARRISON R A, DAVIS C J, et al. The heliospheric imagers onboard the STEREO mission[J]. Solar Phys., 2009, 254(2):387-445
[5]	THOMPSON W T, DAVILA J M, FISHER R R, et al. COR1 inner coronagraph for STEREO-SECCHI[C]//Proceedings of the SPIE Innovative Telescopes and Instrumentation for Solar Astrophysics. Waikoloa, Hawaii, United States:SPIE, 2003. DOI: 10.1117/12.460267
[6]	LARIO D, ARAN A, GÓMEZ-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(1):41
[7]	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]. Solar Phys., 2014, 289(8):3059-3107
[8]	HE H Q, WAN W. On the east-west longitudinally asymmetric distribution of solar proton events[J]. Mon. Not. Roy. Astron. Soc., 2017, 464(1):85-93
[9]	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, DOI: 10.1088/1674-4527/16/8/122
[10]	DING L G, LI G, JIANG Y, et al. Interaction between two coronal mass ejections in the 2013 May 22 large solar energetic particle event[J]. Astrophys. J. Lett., 2014, 793(2):L35, DOI: 10.1088/2041-8205/793/2/L35
[11]	LIU Y D, LUHMANN J G, KAJDIČ P, et al. Observations of an extreme storm in interplanetary space caused by successive coronal mass ejections[J]. Nat. Commun., 2014, 5:3481, DOI: 10.1038/ncomms4481
[12]	REAMES D V, BARBIER L M, NG C K. The spatial distribution of particles accelerated by coronal mass ejection-driven shocks[J]. Astrophys. J., 1996, 466:473-486
[13]	COHEN C M S, MASON G M, MEWALDT R A, et al. Solar energetic particle characteristics and their dependence on longitude in solar cycle 24[J]. AIP Conf. Proc., 2013, 1539(1):151-154
[14]	DRESING N, GÓMEZ-HERRERO R, KLASSEN A, et al. The large longitudinal spread of solar energetic particles during the 17 January 2010 solar event[J]. Solar Phys., 2012, 281(1):281-300
[15]	PARK J, INNES D E, BUCIK R, et al. The source regions of solar energetic particles detected by widely separated spacecraft[J]. Astrophys. J., 2013, 779(2):184
[16]	QIN G, WANG Y, ZHANG M, et al. Transport of solar energetic particles accelerated by ICME shocks:reproducing the reservoir phenomenon[J]. Astrophys. J., 2013, 766(2):74, DOI: 10.1088/0004-637X/766/2/74
[17]	QIN G, WANG Y. Simulations of a gradual solar energetic particle event observed by HELIOS1, HELIOS2, and IMP8[J]. Astrophys. J., 2015, 809(2):177, DOI:10. 1088/0004-637X/809/2/177
[18]	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(2):1014-1022
[19]	TYLKA A J, COHEN C M S, DIETRICH W F, et al. Onsets and release times in solar particle events[C]//Proceedings of the 28th International Cosmic Ray Conference. Tokyo:International Union of Applied Physics, 2003
[20]	GOPALSWAMY N, XIE H, YASHIRO S, et al. Properties of ground level enhancement events and the associated solar eruptions during solar cycle 23[J]. Space Sci. Rev., 2012, 171(1-4):23-60
[21]	TAN L C, MALANDRAKI O E, REAMES D V, et al. Comparison between path lengths traveled by solar electrons and ions in ground-level enhancement events[J]. Astrophys. J., 2013, 768(1):68, DOI: 10.1088/0004-637X/768/1/68
[22]	KIM R S, CHO K S, LEE J, et al. A refined classification of SPEs based on the multienergy channel observations[J]. J. Geophys. Res. Space Phys., 2014, 119(12):9419-9429
[23]	KIM R S, CHO K S, LEE J, et al. Characteristics of four SPE groups with different origins and acceleration processes[J]. J. Geophys. Res. Space Phys., 2015, 120(9):7083-7093