Comparison between ionospheric disturbances caused by barium and cesium

Zhu Xiao-Li; Hu Yao-Gai; Zhao Zheng-Yu; Zhang Yuan-Nong

doi:10.7498/aps.69.20191266

Abstract

After being released in the ionosphere, alkali-metal atoms will be rapidly photoionized by solar UV, producing positive ions and electrons, and forming artificial plasma cloud. Based on a three-dimensional two-species fluid model, considering both the loss of barium atoms due to photoionization and oxidation and the influence of horizontal wind field in the release region, the spatial-temporal evolution of the artificial plasma cloud is discussed. By taking into account the electromagnetic field force, pressure gradient, particle collisions and ion inertia, the ionospheric disturbance effects caused by barium and cesium are compared with each other. The simulation results show that the alkali metal rapidly expands after being released in the ionosphere, and the generated plasma cloud gradually forms an ellipsoidal structure from the inside to the outside under the constraint of magnetic field with considering no wind. Meanwhile, the expanded plasma cloud pushes away the background oxygen ions, forming an oxygen ion density hole in the release center and two symmetrical density bumps on both sides. In the absence of neutral wind, the plasma cloud is dominated by the movement along magnetic field, while considering the background neutral wind, the plasma cloud and background disturbance area will move along the direction of wind, so that the density gradient of plasma cloud becomes steepening on the upwind side. Although the movement of ion cloud across the magnetic field is constrained, the neutrals can pass through the magnetic field freely, so the ion cloud and neutral cloud will separate from each other slowly. Also, the presence of horizontal wind field will make a greater disturbance to the background oxygen ion. By comparing the simulation results of barium and cesium we can see that, qualitatively, the expansion characteristics of Cs⁺ and Ba⁺ as well as their effects on the background O⁺ are similar. Due to the small diffusion coefficient of cesium, the barium cloud expands more rapidly and the coverage area of Ba⁺ cloud is wider. Because of the large photoionization rate of cesium, the ionization yield of cesium is higher than that of barium when the same mass is released. In addition, the snowplow effect of Cs⁺ is stronger than that of Ba⁺, and the oxygen ion density holes and bumps caused by Cs⁺ are also larger.

Keywords:

Authors and contacts

Ionosphere Laboratory, School of Electronics and Information, Wuhan University, Wuhan 430079, China

Corresponding author: Hu Yao-Gai, yaogaihu@whu.edu.cn

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References

[1]	Foppl H, Haerendel G, Haser L, Lutjens P, Lust R, Melzner F, Meyer B, Neuss H, Rieger E 1967 Planet. Space Sci. 15 357 Google Scholar
[2]	Haerendel G, Foppl H, Melzner F, Neuss H, Rieger E, Stocker J, Bauer O, Hofner H, Loidl J 1986 Nature 320 700 Google Scholar
[3]	Caton R G, Pedersen T R, Groves K M, et al. 2017 Radio Sci. 52 539 Google Scholar
[4]	Huba J D, Bernhardt P A, Lyon J G 1992 J. Geophys. Res. Space Phys. 97 11 Google Scholar
[5]	Lloyd K H, Haerendel G 1973 J. Geophys. Res. 78 7389 Google Scholar
[6]	Morse D L, Destler W W 1973 J. Geophys. Res. 78 7417 Google Scholar
[7]	Bernhardt P A, Roussel-Dupre R A, Pongratz M B, et al. 1987 J. Geophys. Res. 92 5777 Google Scholar
[8]	Zakharov Y P 2002 Adv. Space Res. 29 1335 Google Scholar
[9]	Haerendel G, Lust R, Rieger E 1967 Planet. Space Sci. 15 1 Google Scholar
[10]	Schunk R W, Szuszczewicz E P 1988 J. Geophys. Res. Space Phys. 93 12901 Google Scholar
[11]	Mitchell H G, Fedder J A, Huba J D, Zalesak S T 1985 J. Geophys. Res. Space Phys. 90 11091 Google Scholar
[12]	Rozhansky V A, Veselova I Y, Voskoboynikov S P 1990 Planet. Space Sci. 38 1375 Google Scholar
[13]	Drake J F, Mulbrandon M, Huba J D 1988 Phys. Fluids 31 3412 Google Scholar
[14]	Ma T Z, Schunk R W 1991 J. Geophys. Res. Space Phys. 96 5793 Google Scholar
[15]	Ma T Z, Schunk R W 1994 J. Geophys. Res. 99 6331 Google Scholar
[16]	Mendillo M, Hawkins G S, Klobuchar J A 1975 Science 18734 3
[17]	Klobuchar J A, Abdu M A 1989 J. Geophys. Res. Space Phys. 94 2721 Google Scholar
[18]	Choueiri E Y, Oraevsky V N, Dokukin V S 2001 J. Geophys. Res. 106 25673 Google Scholar
[19]	Bernhardt P A 1979 J. Geophys. Res. 84 793 Google Scholar
[20]	Mendillo M, Semeter J, Noto J 1993 Adv. Space Res. 13 55
[21]	Scales W A, Bernhardt P A, Ganguli G 1994 J. Geophys. Res. 99 373 Google Scholar
[22]	Kolomiitsev O P, Ruzhin Y Y, Egorov I B, Razinkov O G, Cherkashin Y N 1999 Phys. Chem. Earth Part C 24 393 Google Scholar
[23]	黄文耿, 古士芬 2005 空间科学学报 25 254 Google Scholar Huang W G, Gu S F 2005 Chin. J. Space Sci. 25 254 Google Scholar
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[33]	Pressman J, Marrmo F F, Aschenbrand L M 1960 Planet. Space Sci. 2 228 Google Scholar
[34]	Holmgren G, Kintner P M, Kelley M C 1981 Adv. Space Res. 1 311 Google Scholar
[35]	Eliason L, Lundin R, Holmgren G 1988 Adv. Space Res. 8 93
[36]	Bleecker D K, Bogaerts A, Gijbels R, Goedheer W 2004 Phys. Rev. E 69 056409 Google Scholar
[37]	Xing Z, Anbang S, Le T, Guan J Z 2019 AIP Adv. 9 015117 Google Scholar

Cited By

图 1 仿真算法流程图

Figure 1. Flow chart of simulation algorithm.

DownLoad: Full-Size Img PowerPoint

图 2 无中性风场时, 300 km高度释放10 kg钡后钡离子和氧离子的离子数密度分布(x-y平面)　(a) Ba⁺, t = 5 s; (b) Ba⁺, t = 30 s; (c) Ba⁺, t = 200 s; (d) O⁺, t = 5 s; (e) O⁺, t = 30 s; (f) O⁺, t = 200 s

Figure 2. Density distribution of Ba⁺ and O⁺ (in x-y plane) after 10 kg barium released at 300 km while no neutral wind is considered: (a) Ba⁺, t = 5 s; (b) Ba⁺, t = 30 s; (c) Ba⁺, t = 200 s; (d) O⁺, t = 5 s; (e) O⁺, t = 30 s; (f) O⁺, t = 200 s.

DownLoad: Full-Size Img PowerPoint

图 3 无中性风场时, 300 km高度释放10 kg钡后钡离子和氧离子的粒子数密度分布(x-z平面)　(a) O⁺, t = 5 s; (b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Ba⁺, t = 5 s; (e) Ba⁺, t = 30 s; (f) Ba⁺, t = 200 s

Figure 3. Density distribution of Ba⁺ and O⁺ (in x-z plane) after 10 kg barium released at 300 km while no neutral wind is considered: (a) O⁺, t = 5 s; (b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Ba⁺, t = 5 s; (e) Ba⁺, t = 30 s; (f) Ba⁺, t = 200 s.

DownLoad: Full-Size Img PowerPoint

图 4 存在x方向大小为1 km/s的中性风时, 300 km高度释放10 kg钡后钡离子和氧离子的粒子数密度分布(x-z平面)　(a) O⁺, t = 5 s; (b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Ba⁺, t = 5 s; (e) Ba⁺, t = 30 s; (f) Ba⁺, t = 200 s

Figure 4. Density distribution of Ba⁺ and O⁺ (in x-z plane) after 10 kg barium released at 300 km with a neutral wind of 1 km/s in the x direction: (a) O⁺, t = 5 s;(b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Ba⁺, t = 5 s; (e) Ba⁺, t = 30 s; (f) Ba⁺, t = 200 s.

DownLoad: Full-Size Img PowerPoint

图 5 钡中性云团(绿色)和离子云团(蓝色)在释放后30 s时的三维分布示意图

Figure 5. Three-dimensional density distribution of barium neutral cloud (green sphere) and ion cloud (blue sphere) at 30 s after release

DownLoad: Full-Size Img PowerPoint

图 6 存在x方向大小为1 km/s的中性风时, 300 km高度释放10 kg铯的粒子数密度分布(x-z平面)　(a) O⁺, t = 5 s; (b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Cs⁺, t = 5 s; (e) Cs⁺, t = 30 s; (f) Cs⁺, t = 200 s

Figure 6. Density distribution of Cs⁺ and O⁺ (in x-z plane) after 10 kg cesium released at 300 km with a neutral wind of 1 km/s in the x direction: (a) O⁺, t = 5 s; (b) O⁺, t = 30 s; (c) O⁺, t = 200 s; (d) Cs⁺, t = 5 s; (e) Cs⁺, t = 30 s; (f) Cs⁺, t = 200 s.

DownLoad: Full-Size Img PowerPoint

图 7 生成的等离子体云团的密度最大值(a)和背景氧离子的最大扰动值(b)随时间的变化

Figure 7. The maximum density of artificial plasma cloud (a) and the maximum disturbance of background oxygen ion (a) versus time.

DownLoad: Full-Size Img PowerPoint

表 1 主要仿真参数表

Table 1. The main simulation parameters.

参数	数值(来源)
模拟时间	201709151800LT
释放地点	(22°N, 109°E)
释放高度/km	300
磁场强度/nT	38860
温度/K	860
地磁倾角	32.4°
地磁偏角	–1.9°
氧离子数密度/cm^–3	9 × 10⁵
氧原子数密度/cm^–3	3.06 × 10⁹
光电离率	0.0357(Ba)^[18]/0.05(Cs)^[24]
阻尼系数/s^–1	0.0149(Ba)/0.0208(Cs)
扩散系数/10¹⁰ $ \rm cm^2\cdot s^{-1} $	2.94(Ba)/2.17(Cs)
原子极化率/10^–24 cm³	39.7(Ba)/59.6(Cs)

DownLoad: CSV

map

[1]	Foppl H, Haerendel G, Haser L, Lutjens P, Lust R, Melzner F, Meyer B, Neuss H, Rieger E 1967 Planet. Space Sci. 15 357 Google Scholar
[2]	Haerendel G, Foppl H, Melzner F, Neuss H, Rieger E, Stocker J, Bauer O, Hofner H, Loidl J 1986 Nature 320 700 Google Scholar
[3]	Caton R G, Pedersen T R, Groves K M, et al. 2017 Radio Sci. 52 539 Google Scholar
[4]	Huba J D, Bernhardt P A, Lyon J G 1992 J. Geophys. Res. Space Phys. 97 11 Google Scholar
[5]	Lloyd K H, Haerendel G 1973 J. Geophys. Res. 78 7389 Google Scholar
[6]	Morse D L, Destler W W 1973 J. Geophys. Res. 78 7417 Google Scholar
[7]	Bernhardt P A, Roussel-Dupre R A, Pongratz M B, et al. 1987 J. Geophys. Res. 92 5777 Google Scholar
[8]	Zakharov Y P 2002 Adv. Space Res. 29 1335 Google Scholar
[9]	Haerendel G, Lust R, Rieger E 1967 Planet. Space Sci. 15 1 Google Scholar
[10]	Schunk R W, Szuszczewicz E P 1988 J. Geophys. Res. Space Phys. 93 12901 Google Scholar
[11]	Mitchell H G, Fedder J A, Huba J D, Zalesak S T 1985 J. Geophys. Res. Space Phys. 90 11091 Google Scholar
[12]	Rozhansky V A, Veselova I Y, Voskoboynikov S P 1990 Planet. Space Sci. 38 1375 Google Scholar
[13]	Drake J F, Mulbrandon M, Huba J D 1988 Phys. Fluids 31 3412 Google Scholar
[14]	Ma T Z, Schunk R W 1991 J. Geophys. Res. Space Phys. 96 5793 Google Scholar
[15]	Ma T Z, Schunk R W 1994 J. Geophys. Res. 99 6331 Google Scholar
[16]	Mendillo M, Hawkins G S, Klobuchar J A 1975 Science 18734 3
[17]	Klobuchar J A, Abdu M A 1989 J. Geophys. Res. Space Phys. 94 2721 Google Scholar
[18]	Choueiri E Y, Oraevsky V N, Dokukin V S 2001 J. Geophys. Res. 106 25673 Google Scholar
[19]	Bernhardt P A 1979 J. Geophys. Res. 84 793 Google Scholar
[20]	Mendillo M, Semeter J, Noto J 1993 Adv. Space Res. 13 55
[21]	Scales W A, Bernhardt P A, Ganguli G 1994 J. Geophys. Res. 99 373 Google Scholar
[22]	Kolomiitsev O P, Ruzhin Y Y, Egorov I B, Razinkov O G, Cherkashin Y N 1999 Phys. Chem. Earth Part C 24 393 Google Scholar
[23]	黄文耿, 古士芬 2005 空间科学学报 25 254 Google Scholar Huang W G, Gu S F 2005 Chin. J. Space Sci. 25 254 Google Scholar
[24]	黄勇, 时家明, 袁忠才 2011 地球 54 1 Google Scholar Huang Y, Shi J M, Yuan Z C 2011 Chin J. Geophys. 54 1 Google Scholar
[25]	胡耀垓, 赵正予, 张援农 2010 59 8293 Google Scholar Hu Y G, Zhao Z Y, Zhang Y N 2010 Acta Phys. Sin. 59 8293 Google Scholar
[26]	胡耀垓, 赵正予, 张援农 2013 62 209401 Google Scholar Hu Y G, Zhao Z Y, Zhang Y N 2013 Acta Phys. Sin. 62 209401 Google Scholar
[27]	汪四成, 方涵先, 杨升高, 翁利斌 2012 地球物理学研究进展 27 2464 Wang S C, Fang H X, Yang S G 2012 Progress in Geophys. 27 2464
[28]	赵海生, 许正文, 吴振森, 冯杰, 吴健, 徐彬, 徐彤, 胡艳莉 2016 65 209401 Google Scholar Zhao H S, Xu Z W, Wu Z S, Feng J, Wu J, Xu B, Xu T, Hu Y L 2016 Acta Phys. Sin. 65 209401 Google Scholar
[29]	Li L, Xu R L 2002 Chin. Phys. Lett. 19 1214 Google Scholar
[30]	胡耀垓, 赵正予, 张援农 2012 61 089401 Google Scholar Hu Y G, Zhao Z Y, Zhang Y N 2012 Acta Phys. Sin. 61 089401 Google Scholar
[31]	谢良海 2013 博士学位论文(北京: 中国科学院大学) Xie L H 2013 Ph. D. Dissertation (Beijing: University of Chinese Academy of Sciences) (in Chinese)
[32]	Scholer, M 1970 Planet. Space Sci. 18 977 Google Scholar
[33]	Pressman J, Marrmo F F, Aschenbrand L M 1960 Planet. Space Sci. 2 228 Google Scholar
[34]	Holmgren G, Kintner P M, Kelley M C 1981 Adv. Space Res. 1 311 Google Scholar
[35]	Eliason L, Lundin R, Holmgren G 1988 Adv. Space Res. 8 93
[36]	Bleecker D K, Bogaerts A, Gijbels R, Goedheer W 2004 Phys. Rev. E 69 056409 Google Scholar
[37]	Xing Z, Anbang S, Le T, Guan J Z 2019 AIP Adv. 9 015117 Google Scholar

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