Statistical Properties of Alfven Ion Cyclotron Waves and Kinetic Alfven Waves in the Inner Heliosphere

被引:0
作者
Sun, Chang [1 ,2 ,3 ]
Yang, Lei [1 ,2 ,3 ]
Li, Qiu-Huan [4 ,5 ]
Dai, Cun-Li [6 ]
Li, Jian-Ping [7 ]
Cheng, Zheng-Wei [3 ]
Wu, De-Jin [1 ,2 ]
机构
[1] Chinese Acad Sci, Key Lab Planetary Sci, Purple Mt Observ, Nanjing 210023, Peoples R China
[2] Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Peoples R China
[3] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing 100190, Peoples R China
[4] Luoyang Normal Univ, Inst Space Phys, Luoyang 471934, Peoples R China
[5] Luoyang Normal Univ, Henan Key Lab Electromagnet Transformat & Detect, Luoyang 471934, Peoples R China
[6] Nanjing Agr Univ, Coll Sci, Nanjing 210095, Peoples R China
[7] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210023, Peoples R China
基金
中国国家自然科学基金;
关键词
(Sun:) solar wind; plasmas; waves; methods: statistical; SOLAR PROBE OBSERVATIONS; MAGNETIC HELICITY; WIND TURBULENCE; DISSIPATION RANGE; ENERGY-TRANSFER; SCALES; FLUCTUATIONS; POLARIZATION; SIGNATURE; RESONANCE;
D O I
10.1088/1674-4527/ace956
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Alfven ion cyclotron waves (ACWs) and kinetic Alfven waves (KAWs) are found to exist at < 0.3 au observed by Parker Solar Probe in Alfvenic slow solar winds. To examine the statistical properties of the background parameters for ACWs and KAWs and related wave disturbances, both wave events observed by Parker Solar Probe are selected and analyzed. The results show that there are obvious differences in the background and disturbance parameters between ACWs and KAWs. ACW events have a relatively higher occurrence rate but with a total duration slightly shorter than KAW events. The median background magnetic field magnitude and the related background solar wind speed of KAW events are larger than those of ACWs. The distributions of the relative disturbances of the proton velocity, proton temperature, the proton number density, and ss cover wider ranges for ACW events than for KAW events. The results may be important for the understanding of the nature and characteristics of Alfvenic slow solar wind fluctuations at ion scales near the Sun, and provide the information of the background field and plasma parameters and the wave disturbances of ACWs and KAWs for further relevant theoretical modeling or numerical simulations.
引用
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页数:10
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