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The study about the wave mechanism of magnetized dusty plasmas has important value to related experiment, industrial processing and exploring celestial space. The linear and nonlinear fluctuation characteristics of the nonuniform magnetized dust plasma system are researched in this paper. For the homogeneous external magnetic field and the nonuniform environment with density and temperature gradients, a two-dimensional nonlinear dynamic magnetoplasma equation is derived considering the strong impact between dust and neutral particles. The linear dispersion relation is obtained by the linearized method. There are both the damping wave causing by strong collision and the harmonic wave by particle drift. Employing the typical numerical parameters for analysis, the results display that the quantum parameter modifies the system lengths; the real wave frequency is proportion to the drift frequency; the imaginary wave frequency has complex relationship with the collision frequency between dust and neutrals, and the collision of particles causes the dissipation effects to the system. Besides, the analytical solutions of drift shock wave and explosive wave are solved by function change method. The variation about the electrostatic potential with the main physical parameters is discussed in detail. It is shown that the strength of the electrostatic shock wave and the width of the explosive wave increase with increasing the dust density and magnetic field intensity, decrease with increasing the collision frequency, change with the drift velocity. When the space-time phase is small, the electrostatic potential changes quickly; once big enough, the potential tends to be stable value and reaches stable state eventually. Finally, the stability of the system is discussed. It is found that the dusty charge, quantum parameter, drift velocity all appear in the disturbed solution. All these results in the paper show that the strong collision effect, quantum effect, particle drift and magnetic field all play important role to the generation, evolution and stability of drift waves.
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Keywords:
- dusty plasma /
- drift wave /
- dispersion relation /
- stability
[1] Morfill G E, Ivlev A V 2009 Rev. Mod. Phys. 81 1353
Google Scholar
[2] 马锦秀 2006 物理 35 244
Ma J X 2006 Physics 35 244
[3] Merlino R L, Goree J 2004 Phys. Today 57 32
[4] Shukla P K, Mamun A A 2002 Introduction to Dusty Physics Plasmas (Bristol: Institute of Physics) pp29−35
[5] Verheest F 2000 Waves in Dusty Space Plasmas (Dordrecht: Kluwer Academic Publishers, The Netherlands) pp11−56
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Google Scholar
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Google Scholar
[9] Merlino R L 2014 J. Plasma Phys. 80 773
Google Scholar
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Google Scholar
[12] Haas F 2005 Phys. Plasmas 12 062117
Google Scholar
[13] Haque Q, Mahmood S 2008 Phys. Plasmas 15 034501
Google Scholar
[14] Masood W 2009 Phys. Lett. A 373 1455
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[15] Masood W, Karim S, Shah H A, Siddiq M 2009 Phys. Plasmas 16 042108
Google Scholar
[16] Yang J R, Lv K, Xu L, Mao J J, Liu X Z, Liu P 2017 Chin. Phys. B 26 065200
[17] Yang J R, Wu B, Mao J J, Liu P, Wang J Y 2014 Commun. Theor. Phys 62 871
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Google Scholar
[19] Sadiq M, Ali S, Sabry R 2009 Phys. Plasmas 16 013706
Google Scholar
[20] Sharma P, Patidar A, Jain S, Vyas B 2018 Phys. Plasmas 25 083714
Google Scholar
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Google Scholar
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[23] Mehdipoor M 2020 The Eur. Phys. J. Plus 135 299
Google Scholar
[24] Masood W, Karim S, Shah H A 2010 Phys. Scr. 82 045503
Google Scholar
[25] Kato S 1968 Astrophys. Space Sci. 2 37
Google Scholar
[26] Dev A N, Deka M K, Sarma J, Adhikary N C 2015 J. Korean Phys. Soc. 67 339
Google Scholar
[27] Khan S A, Mushtaq A, Masood W 2008 Phys. Plasmas 15 013701
Google Scholar
[28] Smith B A, Soderblom L, Beebe R, et al. 1981 Science 212 163
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Google Scholar
[30] Humes D H 1980 J. Geophys. Res. 85 5841
Google Scholar
[31] Yang J R, Xu T, Mao J J, Liu P, Liu X Z 2017 Chin. Phys. B 26 015202
Google Scholar
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图 5 (15)式虚色散频率随着波数k和碰撞频率
$ \nu_{\rm {dn}} $ 的变化,$\theta = {{\text{π}}}/{3}$ , 对应的其他参量见(11)式Figure 5. Variation of the imaginary dispersion frequency with the wave number k and the collision frequency
$ \nu_{\rm {dn}} $ determined by Eq. (15) for$\theta = {{\text{π}}}/{3}$ . Other parameters are given in Eq. (11).
图 10 (19)式爆炸波
$ \varPhi_2 $ 随着尘埃密度$ n_{\rm d} $ 的变化. 对应的参量为$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ n_{\rm d} = 1.2\times10^{18}{\ \rm{cm}^{-3}} $ (实线),$ n_{\rm d} = 1.4\times10^{18}{\ \rm{cm}^{-3}} $ (虚线), 其他参量见(11)式Figure 10. Profile of the explosive wave
$ \varPhi_2 $ by Eq. (19) with$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ n_{\rm d} = 1.2\times10^{18}{\ \rm{cm}^{-3}} $ (solid line), and$ n_{\rm d} = 1.4\times10^{18}{\ \rm{cm}^{-3}} $ (dash line). Other parameters are given in Eq. (11).
图 11 (19)式爆炸波
$ \varPhi_2 $ 随着碰撞频率$ \nu_{\rm {dn}} $ 的变化. 对应的参量为$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ \nu_{\rm {dn}} = 10^{6}\ \rm{Hz} $ (实线),$ \nu_{\rm {dn}} = 3\times 10^{6}\ \rm{Hz} $ (虚线), 其他参量见(11)式Figure 11. Profile of the explosive wave
$ \varPhi_2 $ given by Eq. (19) with$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ \nu_{\rm {dn}} = 10^{6}\ \rm{Hz} $ (solid line), and$ \nu_{\rm {dn}} = 3\times10^{6}\ \rm{Hz} $ (dash line). Other parameters are given in Eq. (11).
图 12 (19)式爆炸波
$ \varPhi_2 $ 随着漂移速度v的变化. 对应的参量为$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ v = 10^{3}\ \rm{cm/s} $ (实线),$ v = 10^{4}\ \rm{cm/s} $ (虚线), 其他参量见(11)式Figure 12. Profile of the explosive wave
$ \varPhi_2 $ given by Eq. (19) with$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ v = 10^{3}\ \rm{cm/s} $ (solid line), and$ v = 10^{4}\ \rm{cm/s} $ (dash line). Other parameters are given in Eq. (11).
图 13 (19)式爆炸波
$ \varPhi_2 $ 随着磁场强度$ B_0 $ 的变化. 对应的参量为$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ B_0 = 10^{8}\ \rm{G} $ (实线), 和$ B_0 = 3\times 10^{8}\ \rm{G} $ (虚线), 其他参量见(11)式Figure 13. Profile of the explosive wave
$ \varPhi_2 $ given by Eq. (19) with$ k_{2} = 2 $ ,$ k_{3} = 1 $ ,$ B_0 = 10^{8}\ \rm{G} $ (solid line), and$ B_0 = 3\times10^{8}\ \rm{G} $ (dash line). Other parameters are given in Eq. (11). -
[1] Morfill G E, Ivlev A V 2009 Rev. Mod. Phys. 81 1353
Google Scholar
[2] 马锦秀 2006 物理 35 244
Ma J X 2006 Physics 35 244
[3] Merlino R L, Goree J 2004 Phys. Today 57 32
[4] Shukla P K, Mamun A A 2002 Introduction to Dusty Physics Plasmas (Bristol: Institute of Physics) pp29−35
[5] Verheest F 2000 Waves in Dusty Space Plasmas (Dordrecht: Kluwer Academic Publishers, The Netherlands) pp11−56
[6] Shukla P K 2002 Dust Plasma Interaction in Space (New York: Nova Science) pp156−159
[7] Liang Z F, Tang X Y 2013 Commun. Nonlinear Sci. Numer. Simul. 18 3014
Google Scholar
[8] Barkan A, Merlino R L, Angelo N D 1995 Phys. Plasmas 2 3563
Google Scholar
[9] Merlino R L 2014 J. Plasma Phys. 80 773
Google Scholar
[10] Rao N N, Shukla P K, Yu M Y 1990 Planet. Space Sci. 18 543
[11] Shukla P K, Rahman H U 1996 Phys. Plasmas 3 430
Google Scholar
[12] Haas F 2005 Phys. Plasmas 12 062117
Google Scholar
[13] Haque Q, Mahmood S 2008 Phys. Plasmas 15 034501
Google Scholar
[14] Masood W 2009 Phys. Lett. A 373 1455
Google Scholar
[15] Masood W, Karim S, Shah H A, Siddiq M 2009 Phys. Plasmas 16 042108
Google Scholar
[16] Yang J R, Lv K, Xu L, Mao J J, Liu X Z, Liu P 2017 Chin. Phys. B 26 065200
[17] Yang J R, Wu B, Mao J J, Liu P, Wang J Y 2014 Commun. Theor. Phys 62 871
[18] Moslem W M, Shukla P K, Ali S, Schlickeiser R 2007 Phys. Plasmas 14 042107
Google Scholar
[19] Sadiq M, Ali S, Sabry R 2009 Phys. Plasmas 16 013706
Google Scholar
[20] Sharma P, Patidar A, Jain S, Vyas B 2018 Phys. Plasmas 25 083714
Google Scholar
[21] Jorge R, Ricci P, Loureiro N F 2018 Phys. Rev. Lett. 121 165001
Google Scholar
[22] Kumar A, Das A, Kaw P 2019 Phys. Plasmas 26 8
[23] Mehdipoor M 2020 The Eur. Phys. J. Plus 135 299
Google Scholar
[24] Masood W, Karim S, Shah H A 2010 Phys. Scr. 82 045503
Google Scholar
[25] Kato S 1968 Astrophys. Space Sci. 2 37
Google Scholar
[26] Dev A N, Deka M K, Sarma J, Adhikary N C 2015 J. Korean Phys. Soc. 67 339
Google Scholar
[27] Khan S A, Mushtaq A, Masood W 2008 Phys. Plasmas 15 013701
Google Scholar
[28] Smith B A, Soderblom L, Beebe R, et al. 1981 Science 212 163
Google Scholar
[29] Smith B A, Soderblom L, Batson R, et al. 1982 Science 215 504
Google Scholar
[30] Humes D H 1980 J. Geophys. Res. 85 5841
Google Scholar
[31] Yang J R, Xu T, Mao J J, Liu P, Liu X Z 2017 Chin. Phys. B 26 015202
Google Scholar
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