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Plasma bubbles in the ionosphere have a significant effect on radio wave communication and navigation. Under the worst condition, it will fail to function the systems relying on the ionosphere. On the other hand, the physical mechanisms of evolution and diurnal variations of the plasma bubbles in the ionosphere are still unclear. Therefore, it is still worthy to simulate the plasma bubbles in the ionosphere for radio wave propagation and science. In this study, the equatorial plasma bubbles induced by one- and two- dimensional disturbance in the ionosphere are simulated, where traveling ionospheric disturbance (TID) is used to produce the two-dimensional disturbance in the ionosphere. The dispersion relationship of gravity wave is used to represent the corresponding wavelength of TID in this study. More importantly, we investigate the effect of recombination rate on the development of plasma bubbles by numerical simulation. The simulation results show that the recombination rate of the plasma in the ionosphere has a significant effect on the development of plasma bubbles. The greater the recombination rate, the more time it takes to produce the plasma bubbles. For one-dimensional disturbance in the ionosphere, there is no significant effect in the structure of plasma bubbles for the recombination rate of the plasma. However, the recombination rate plays a significant effect on the structure of plasma bubbles induced by TID. When the recombination rate is less in numerical simulation, the complex structure including bifurcation, plume-like structures, and pinching of plasma bubbles can occur in the development of bubbles. In contrast, the structure of plasma bubbles is simpler when the recombination rate is greater in simulation. As a result, the recombination rate of the plasma is a significant factor for simulating the plasma bubbles in the ionosphere. The greater recombination rate can result in the slowing down of equatorial plasma bubbles and the simplifying the structure of the bubbles as well. In addition, it is found that not all of plasma bubbles at the bottom of the ionosphere can grow to the top of the ionosphere when many bubbles occur on the bottom side. The direction of the polarization electric field near the bubbles can be changed in the non-linear development of the bubbles. Therefore, only the bubbles where the polarization electric field is always eastward can develop to the topside.
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Keywords:
- chemical recombination rate /
- equatorial plasma bubble /
- travelling ionospheric disturbances /
- numerical simulation
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Google Scholar
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Google Scholar
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图 1 水平东向电场值随高度的变化
Figure 1. Altitudinal variation of eastward electrical field in the simulation.
图 2 背景电离层电子密度剖面
Figure 2. Electron density profile in the background ionos phere.
图 3 存在TIDs(波长为300 km, 周期为40 min)扰动的背景电离层
Figure 3. Background ionosphere with TIDs (horizontal wavelength is 300 km and period is 40 min).
图 4
$\alpha = 1$ 时一维正弦扰动产生等离子体泡的发展过程Figure 4. Evolution of plasma bubbles caused by one dimensional disturbance with
$\alpha = 1$ .
图 6
$\alpha = 0.01$ 时一维正弦扰动产生等离子体泡的发展过程Figure 6. Evolution of plasma bubbles caused by one dimensional disturbance with
$\alpha = 0.01$ .
图 5
$\alpha = 0.1$ 时一维正弦扰动产生等离子体泡的发展过程Figure 5. Evolution of plasma bubbles caused by one dimensional disturbance with
$\alpha = 0.1$ .
图 7
$\alpha = 1$ 时TIDs产生等离子体泡的发展过程Figure 7. Evolution of plasma bubbles caused by TIDs with
$\alpha = 1$ .
图 8
$\alpha = 0.1$ 时TIDs产生等离子体泡的发展过程Figure 8. Evolution of plasma bubbles caused by TIDs with
$\alpha = 0.1$ .
图 9
$\alpha = 0.01$ 时TIDs产生等离子体泡的发展过程Figure 9. Evolution of plasma bubbles caused by TIDs with
$\alpha = 0.01$ .
图 10
$\alpha = 0$ 时TIDs产生等离子体泡的发展过程Figure 10. Evolution of plasma bubbles caused by TIDs with
$\alpha = 0$ . -
[1] Dungey J W 1956 J. Atmos. Terr. Phys. 9 304
Google Scholar
[2] Abdu M A 2001 J. Atmos. Terr. Phys. 63 869
Google Scholar
[3] Tsunoda R T, Yamamoto M, Tsugawa T, Hoang T L, Ram S T, Thampi S V, Chau H D, Nagatsuma T 2011 Geophys. Res. Lett. 38 L20102
Google Scholar
[4] Sekar R, Suhasini R, Raghavarao R 1994 J. Geophys. Res. 99 2205
Google Scholar
[5] Huang C S, Kelley M C 1996 J. Geophys. Res. Space Physics 101 303
Google Scholar
[6] Hysell D L, Kelley M C, Swartz W E, Woodman R F 1990 J. Geophys. Res. Space Physics 95 17253
Google Scholar
[7] Huang C S, Kelley M C 1996 J. Geophys. Res. Space Physics 101 293
Google Scholar
[8] Scannapieco A J, Ossakow S L 1976 Geophys. Res. Lett. 3 451
Google Scholar
[9] Zalesak S T, Ossakow S L 1980 J. Geophys. Res. 85 2131
Google Scholar
[10] Zalesak S T, Ossakow S L, Chaturvedi P K 1982 J. Geophys. Res. 87 151
Google Scholar
[11] 谢红, 肖佐 1993 地球物理学报 36 18
Google Scholar
Xie H, Xiao Z 1993 Chinese J. Geophys. 36 18
Google Scholar
[12] 高泽, 方涵先, 汪四成, 杨升高 2017 地球物理学报 60 470
Google Scholar
Gao Z, Fang H X, Wang S C, Yang S G 2017 Chinese J. Geophys. 60 470
Google Scholar
[13] Huba J D, Joyce G, Krall J 2008 Geophys. Res. Lett. 35 10102
Google Scholar
[14] Yokoyama T, Shinagawa H, Jin H 2014 J. Geophys. Res. Space Physics 119 10474
[15] Yokoyama T 2017 Prog. in Earth and Planet. Sci. 4 37
Google Scholar
[16] Krall J, Huba J D, Ossakow S L, Joyce G, Makela J J, Miller E S, Kelley M C 2011 Geophys. Res. Lett. 38 L08103
[17] Krall J, Huba J D, Fritts D C 2013 Geophys. Res. Lett. 40 661
Google Scholar
[18] Hines C O 1960 Can. J. Phys. 38 1441
Google Scholar
[19] Alfonsi L, Spogli L, Pezzopane M, Romano V, Zuccheretti E, De Franceschi G, Cabrera M A, Ezquer R G 2013 J. Geophys. Res. Space Physics 118 4483
Google Scholar
[20] Jiang C, Yang G, Deng C, Zhou C, Zhu P, Yokoyama T, Song H, Lan T, Ni B, Zhao Z, Zhang Y 2015 J. Geophys. Res. Space Physics 120 10979
Google Scholar
[21] Jiang C, Yang G, Liu J, Zhao Z 2019 J. Geophys. Res. Space Physics 124 1317
Google Scholar
[22] Sultan P J 1996 J. Geophys. Res. 101 26875
Google Scholar
[23] Kelley M C 2009 Introduction to Spatial Econometrics (2nd ed.), (Amsterdams: Elsevier) p 99
[24] Lanchester B S, Nygren T, Jarvis M J, Edwards R 1993 Ann. Geophys. 11 925
[25] Miyoshi Y, Jin H, Fujiwara H, Shinagawa H 2018 J. Geophys. Res. Space Physics 123 2141
[26] Abdu M A, Batista I S, Kantor I J, Sobral J H A 1982 J. Atmos. Terr. Phys. 44 759
Google Scholar
[27] Fukumitsu K, Yabe T, Ogata Y, Oami T, Ohkubo T 2015 J. Comput. Phys. 286 62
Google Scholar
[28] Yokoyama T, Jin H, Shinagawa H 2015 J. Geophys. Res. Space Physics 120 8810
Google Scholar
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