Assessment of applicability of cold plasma dispersion relation of slot region hiss based on Van Allen Probes observations

Zhu Qi; Ma Xin; Cao Xing; Ni Bin-Bin; Xiang Zheng; Fu Song; Gu Xu-Dong; Zhang Yuan-Nong

doi:10.7498/aps.71.20211671

Abstract

Electron scattering caused by plasmapheric hiss is the dominant mechanism that is responsible for the formation of slot region (1.8 ≤ L ≤ 3) between the Earth’s inner and outer radiation belts. The cold plasma dispersion relation of plasmaspheric hiss is widely used to quantify its scattering effect on energetic electrons. However, the existence of hot plasmas in the realistic magnetospheric environment will modify the dispersion properties of plasmaspheric hiss. According to Van Allen Probes observations, we select all hiss events in the slot region and compare the observed hiss wave amplitudes with the converted hiss wave amplitudes deduced from cold plasma dispersion relation and electric field observations, and then study the dependence of the applicability of cold plasma dispersion relation of slot region hiss on spatial position and geomagnetic activity. The results show that the cold plasma approximation tends to overestimate the amplitude of slot region hiss. The difference between the observed amplitude and the converted hiss wave amplitude has a strong day night asymmetry. However, it shows a slight dependence on the level of geomagnetic activities. In addition, we find that the converted wave magnetic field intensity is significantly lower (higher) than the observed magnetic field intensity at lower frequencies (higher frequencies), which indicates that the cold plasma approximation generally overestimates (underestimates) the scattering effects of hiss waves on the lower (higher) energy electrons in the slot region. Our study confirms that the application scope of the cold plasma dispersion relation of slot hiss has strong spatial and frequency limitations, which is of great importance in deepening our understanding of the dynamic evolution of electrons in the slot region.

Keywords:

Authors and contacts

1.
School of Electronic Information, Wuhan University, Wuhan 430072, China
2.
Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei 230026, China

Corresponding author: Cao Xing, cxing@whu.edu.cn ; Ni Bin-Bin, bbni@whu.edu.cn ;

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 42025404, 41904143, 41904144), the B-type Strategic Priority Program of the Chinese Academy of Sciences (Grant No. XDB41000000), and the China Postdoctoral Science Foundation (Grant Nos. 2020M672405, 2019M662700).

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References

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Cited By

图 1 2015年5月23日范阿伦B观测到的嘶声波事件　(a)背景电子密度; (b) AE和Dst指数; (c)观测电场功率谱密度; (d)观测磁场功率谱密度; (e) 基于冷等离子理论的反演磁场功率谱密度; (f)传播角; (g)极化率; (h)平面度; (i)嘶声波观测(红色)和反演(蓝色)幅值. 图(c)—(e)中的品红线条对应下混杂频率f_LHR

Figure 1. Overview of a plasmaspheric hiss event observed by Van Allen Probe B on 23 May 2015: (a) Ambient electron density; (b) AE index and SYM_H index; observed power spectral intensity of (c) electric field and (d) magnetic field; (e) converted power spectral intensity of magnetic field based on the cold plasma dispersion relation; (f) wave normal angle; (g) wave ellipticity; (h) wave planarity; (i) observed (red) and converted (blue) hiss wave amplitudes. The magenta lines in panels (c)–(e) correspond to the lower hybrid resonance frequency f_LHR.

DownLoad: Full-Size Img PowerPoint

图 2 嘶声波观测幅值与反演幅值比值(${\rm{log}}_{10}\left( {{B}_{\rm{obs}}}/{{B}_{\rm{cvt}}}\right)$)的(a)均值与(b)方差随L和MLT的全球二维统计分布; (c)—(f)比值的均值与方差在不同MLT区间随L-shell的一维统计分布; (g)—(j)在不同L-shell区间随MLT的一维统计分布

Figure 2. Global distribution of the (a) mean value and (b) variance of the ratio of observed hiss amplitudes and converted amplitudes (${\rm{log}}_{10}\left( {{B}_{\rm{obs}}}/{{B}_{\rm{cvt}}}\right)$) as a function of L-shell and MLT; (c)–(f) the mean value and variance of the ratio as a function of L-shell in different MLT sectors; (g)–(j) the mean value and variance of the ratio as a function of MLT in different L-shell ranges.

DownLoad: Full-Size Img PowerPoint

图 3 不同地磁活动水平下, 嘶声波观测幅值与反演幅值比值(${\rm{log}}_{10}\left( {{B}_{\rm{obs}}}/{{B}_{\rm{cvt}}}\right)$)的均值和方差随L和MLT的全球统计分布(a)—(c)均值; (d)—(f)方差

Figure 3. From left to right, global distribution of the mean value and variance of the ratio of observed hiss amplitudes and converted amplitudes (${\rm{log}}_{10}\left( {{B}_{\rm obs}}/{{B}_{\rm cvt}}\right)$) as a function of L-shell and MLT, in different geomagnetic conditions: (a)–(c) mean value; (d)–(f) variance of the ratio.

DownLoad: Full-Size Img PowerPoint

图 4 嘶声波观测的磁场功率谱密度与反演的磁场功率谱密度比值(${\rm{log}}_{10}\left( {{B}_{\rm{obs}}}/{{B}_{\rm{cvt}}}\right)$)的均值(蓝线)和方差(红线)随波动频率的变化

Figure 4. Mean value (blue) and variance (red) of the ratio of observed and converted power spectral intensity $( {\rm{log}}_{10}\left( {{B}_{\rm{obs}}}/{{B}_{\rm{cvt}}}\right)$) as a function of wave frequency.

DownLoad: Full-Size Img PowerPoint

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[30]	Cao X, Ni B B, Summers D, Zou Z, Fu S, Zhang W 2017 Geophys. Res. Lett. 44 9547 Google Scholar
[31]	Fu S, Yi J, Ni B, Zhou R, Hu Z, Cao X, Gu X, Guo D 2020 Geophys. Res. Lett. 47 e2020GL086963 Google Scholar
[32]	Ni B, Huang H, Zhang W, Gu X, Zhao H, Li X, Baker D, Fu S, Xiang Z, Cao X 2019 Geophys. Res. Lett. 46 4134 Google Scholar
[33]	Zhao H, Ni B, Li X, Baker D N, Johnston W R, Zhang W, Xiang Z, Gu X, Jaynes A N, Kanekal S G, Blake J B, Claudepierre S G, Temerin M A, Funsten H O, Reeves G D, Boyd A J 2019 Nat. Phys. 15 367 Google Scholar
[34]	Claudepierre S G, Ma Q, Bortnik J, O'Brien T P, Fennell J F, Blake J B 2020 Geophys. Res. Lett. 47 e2019GL086056 Google Scholar
[35]	Kennel C F, Engelmann F 1966 Phys. Fluids 9 2377 Google Scholar
[36]	Xiao F L, Su Z, Zheng H. Wang S 2009a J. Geophys. Res. Space Phys. 114 A03201 Google Scholar
[37]	Xiao F L, Zong Q G, Chen L 2009b J. Geophys. Res. Space Phys. 114 A01215 Google Scholar
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[40]	Zhu Q, Cao X, Gu X, N i, B, Xiang Z, Fu S, Summers D, Hua M, Lou Y, Ma X, Guo Y, Guo D, Zhang W 2021 J. Geophys. Res. Space Phys. 126 A029057 Google Scholar
[41]	Reeves G D, Fritz T A, Cayton T E, Belian R D 1990 Geophys. Res. Lett. 17 2015 Google Scholar
[42]	Friedel R H W, Korth A, Kremser G 1996 J. Geophys. Res. Space Phys. 101 A00399 Google Scholar
[43]	Baker D N, Pulkkinen T I, Hesse M, Mcpherron R L 1997 J. Geophys. Res. Space Phys. 102 A03961 Google Scholar
[44]	Cao J B, Wei X H, Duan A Y, Fu H S, Zhang T L, Reme H, Dandouras I 2013 J. Geophys. Res. Space Phys. 118 1659 Google Scholar
[45]	Chen L, Thorne R M, Shprits Y, Ni B 2013 J. Geophys. Res. Space Phys. 118 2185 Google Scholar
[46]	Turner D L, Claudepierre S G, Fennell J F, O'Brien T P, Blake J B, Lemon C, Gkioulidou M, Takahashi K, Reeves G D, Thaller S, Breneman A, Wygant J R, Li W, Runov A, Angelopoulos V 2015 Geophys. Res. Lett. 42 2079 Google Scholar
[47]	Cao X, Shprits Y, Ni B, Zhelavskaya I S 2017 Sci. Rep. 7 17719 Google Scholar
[48]	Ni B, Cao X, Shprits Y Y, Summers D, Gu X, Fu S, Lou Y 2018 Geophys. Res. Lett. 45 21 Google Scholar
[49]	Yu J, Li L Y, Cui J, Cao J B, Wang J 2019 Geophys. Res. Lett. 46 6306 Google Scholar
[50]	Yu J, Li L Y, Cui J, Cao J B, Wang J, He Z, Yang J 2020 J. Geophys. Res. Space Phys. 125Google Scholar
[51]	Hartley D P, Kletzing C A, Kurth W S, Bounds S R, Averkamp T F, Hospodarsky G B, Wygant J R, Bonnell J W, Santolík O, Watt C E J 2016 J. Geophys. Res. Space Phys. 121 4590 Google Scholar
[52]	Cao X, Ni B, Summers D, Fu S, Gu X, Shi R 2020 Astrophys. J. 896 118 Google Scholar
[53]	Ma X, Cao X, Ni B, Zhu Q, Xiang Z 2021 Astrophys. J. 916 Google Scholar
[54]	Selesnick R S, Blake J B, Mewaldt R A 2003 J. Geophys. Res. Space Phys. 108 1468 Google Scholar
[55]	Kim K C, Shprits Y, Subbotin D, Ni B 2011 J. Geophys. Res. Space Phys. 116 A10214 Google Scholar
[56]	Meredith N P, Horne R B, Glauert S A, Anderson R R 2007 J. Geophys. Res. Space Phys. 112 8214 Google Scholar
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Vol. 71, Issue 5 - 2022-03-05

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