Exact solutions of dispersion equation for MHD waves with shortwavelength modification


 Griselda Daniels
 1 years ago
 Views:
Transcription
1 Article Astrophysics April 011 Vol. 56 No. 10: doi: /s Exact solutions of dispersion equation for MHD waves with shortwavelength modification CHEN Ling 1, & WU DeJin 1* 1 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 10008, China; Graduate University of Chinese Academy of Sciences, Beijing 10001, China Received August 30, 010; accepted November 9, 010 Dispersive magnetohydrodynamic MHD) waves with shortwavelength modification have an important role in transforming energy from waves into particles. In this paper, based on the twofluid mode, a dispersion equation, including the shortwavelength effect, and its exact solution are presented. The outcome is responsible for the shortwavelength modification versions of the three ideal MHD modes i.e. the fast, slow and ). The results show that the fast and modes are modified considerably by the shortwavelength effect mainly in the quasiparallel and quasiperpendicular propagation directions, respectively, while the slow mode can be affected by the shortwavelength effect in all propagation directions. On the other hand, the dispersive modification occurs primarily in the finite regime of 01 < < 1 for the fast mode and in the high regime of 0.1 < < 10 for the slow mode. For the mode, the dispersive modification occurs from the low regime of < 01 through the high regime of > 1. plasma, MHD waves, shortwavelength effect, dispersion relation Citation: Chen L, Wu D J. Exact solutions of dispersion equation for MHD waves with shortwavelength modification. Chinese Sci Bull, 011, 56: , doi: /s It is well known that there are three ideal magnetohydrodynamic MHD) modes: the fast, slow and waves in the lowfrequency limit much lower than the ion cyclotron frequency ω ci ) and the longwavelength limit much longer than the ion Larmor radius ρ i ). When wavelengths reduce to the characteristic length scales, such as λ e and ρ i, where λ e is the electron inertial length, the ions are free while the electrons are tightly bound to magnetic field lines because their Larmor radius is much smaller than that of the ions i.e. ρ e ρ i ). This leads to the presence of spatial charge and the dispersion of the MHD waves. In the case of the wave, the dispersive wave is called the kinetic wave KAW). In the KAW, the perturbed electric fields have a nonero component parallel to the background magnetic field that may cause efficient heating and acceleration of the plasma particles [1 4]. KAWs have been extensively discussed because of their potential importance in the particle energiation of plasmas. *Corresponding author Also, they have been applied to laboratory, space and astrophysical plasmas, such as tokamak plasma heating [5 7], auroral electron acceleration [8 11], solar coronal plasma heating [1 14], and abnormal heating of heavy ions in the extended corona [15,16]. On the other hand, the other two modes, the fast and slow waves, have been given little attention. Some recent studies on the MHD turbulence in interstellar and interplanetary spaces show that the energy cascades primarily by developing smallscales structures perpendicular to the local field, with k k [17 0]. Large values of k could be the consequence of refraction [1,], resonant absorption [3 5], and turbulent cascade [6]. This result is supported by numerical simulations of magnetied turbulence with a dynamically strong mean field [7,8]. In situ measurements of turbulence in the solar wind and observations of interstellar scintillation also show similar evidence for the theoretical results above [9 34]. For a warm plasma with a high of ie) 1, which is the case for the solar wind and the magnetosheath, the compression wave is coupled with the acoustic wave and leads c The Authors) 011. This article is published with open access at Springerlink.com csb.scichina.com
2 956 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No. 10 to fast and slow magnetosonic waves. In particular, the fact that the ion thermal speed is v Ti v A the velocity) indicates that the ion gyroradius ρ i is comparable to the ion inertial length λ i. This implies that the shortwavelength effect can considerably modify the dispersion relations of the fast and slow magnetosonic waves, as well as modifying the dispersion relation of the shear wave, such as the case of KAWs. Some theoretical studies of MHD turbulence cascades in the solar wind show that the fluctuations in the MHD modes and their collisionless Landau damping are responsible for the steeping of the MHD turbulence spectrum at higher wavenumbersk i.e. shortwavelengths) [6,35 38]. Recently, similar lowfrequency phenomena has been investigated by many authors, for example, the ionospheric dynamo [39], shock arrival time [40], the response of magnetosphere to interplanetary shock [41,4], suprathermal particle events [43], distribution of fieldaligned current carried by waves [44], the behavior of plasma armature [45] and MHD processes of flight vehicles [46 48]. In this paper, we derive an exact dispersion equation, based on the twofluid model, which contains all three MHD modes with the shortwavelength modification. Furthermore, based on the dispersion equation, we present the dispersion relations, which are the versions, with shortwavelength modification, of the three modes: the fast and slow magnetosonic waves and the shear wave. The effects of the propagation angle, the shortwavelength modification and the plasma beta on the three dispersive waves are also discussed. 1 Dispersion equation in the twofluid model In a protonelectron plasma, which is magnetied by a uniform magnetic field B 0 along the direction, the complete set of twofluid equations can be written as follows: t + v i )n i + n i v i = 0, 1) t + v e )n e + n e v e = 0, ) t + v i )v i = e m i E + v i B) 1 m i n i p i, 3) t + v e )v e = e m e E + v e B) 1 m e n e p e, 4) t + v i )p i n γ i i ) = 0, 5) t + v e )p e n γ e e ) = 0, 6) E = t B, 7) B = µ 0 en i v i n e v e ) + ɛ 0 µ 0 t E, 8) where E is the electric field, B the magnetic field, t the partial derivative with respect to the time t, the 3dimensional spatial gradient operator, e the elementary charge, µ 0 the permeability of free space, ɛ 0 the permittivity of free space, m ei), n ei), v ei), p ei), and γ ei) are the electron ion) mass, density, velocity, thermal pressure, and polyindex, respectively, α is the angle between the wave vector k and the ambient magnetic field B 0 i.e. the axis). We mark the unperturbed and perturbed quantities with the subscript 0 and the prefix δ, respectively. For onedimensional plane waves propagating in the x plane, with wave vector k x, 0, k ) and the frequency ω, all the perturbed quantities vary in the form: δ f exp [ i ωt k x x k ) ]. The lineariing perturbed velocities of the ions and electrons can be obtained as follows: ) ω δv i δv i = 1 δe B 0 iδp ) i ω ci B 0 ) ω δv e δv e = 1 ω ce B 0 iq iω m i ω ci q i n i0 k B 0 δe iδp ik q i n i0 δe B 0 iδp e iq eω m e ω ce ), 9) q e n e0 k B 0 δe iδp e k q e n e0 ) ), 10) where the unperturbed velocity v 0 = 0 and the lowfrequency limit ω ω ci ) have been used. We neglect the contribution of the polariation drifts of the electrons the last parenthesis term in the transverse components of 10)) compared to that of the ions. The pressure perturbations may be obtained from eqs. 5) and 6): δp i = γ i T i0 δn i, δp e = γ e T e0 δn e, 11) where the density perturbations δn i and δn e follow from eqs. 1) and ): δn i = n i0 k δv i ω, δn e = n e0 k δv e ω. 1) Following Wu [49], for the lowfrequency and the nonrelativistic cases, in which the Maxwell s displacement current term, on the righthand side of eq. 8), may be neglected, equating Faraday s Law and Ampere s Law yields a dispersion tensor of the form Λ E = 0. The dispersion equation can then be obtained by calculating Λ = 0 as follows: where the coefficients Ω 6 AΩ 4 + BΩ C = 0, 13) A = K A + k k + C; B = k K A + C; C = 1 + Q + k λ e k In the expressions above, the parameter K A 1 + Q + k ρ s 1 + Q + k λ e. 14) 15) is the coefficient of the KAW dispersion relation, Ω = K A [3,39], in a low plasma, where Ω ω/k v A ) is the wave frequency in units of frequency k v A ). The other parameters are v s γ i T 0i + γ e T 0e )/m i : the ion acoustic
3 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No speed, ρ s v s /ω ci : the ion acoustic gyroradius, λ e c/ω pe : the electron inertial length, ω pe n 0 e /m e ɛ 0 : the electron plasma frequency, v s/v A = i + e : the ratio of the total thermal pressure to the magnetic pressure, Q m e /m i : the ratio of the electron mass to the ion mass, and k = k + k : the total wavenumber. Finally, we note that in the derivation of the dispersion eq. 13), we have used the quasineutrality condition n i n e. Solutions with the shortwavelength modification The dispersion eq. 13) can be rewritten as the standard form of the Cardan equation, that is where Ω Ω 0 )3 + pω Ω 0 ) + q = 0, 16) p = B 3Ω 4 0, q = Ω6 0 + BΩ 0 C 17) with the parameter Ω 0 = A/3. When the discriminant q /4 + p 3 /7 < 0, the Cardan eq. 16) has three real roots as follows: Ω F = Ω 0 + R cos θ 3, 18) and where R = Ω S = Ω 0 Ω A = Ω 0 Ω 4 0 B 3 ; θ + π + R cos, 19) 3 θ + 4π + R cos, 0) 3 q θ = arccos R. 1) 3 In the longwavelength limit of k λ e and k ρ s 1, one has A ) k k, B 1 + ) k k, C k, ) and K A 1. As a consequence, from eqs. 18) 0), the three roots of the Cardan eq. 16) in the longwavelength limit are Ω F k ) k, 3) Ω S k ) k, 4) and Ω A 1. 5) These are the dispersion relations for the ideal MHD modes i.e. the fast and slow magnetosonic waves and the shear wave). Therefore, the three roots, in eqs. 18) 0), k of the Cardan eq. 16) are the modified versions, including the shortwavelength effects, of the dispersion relations for the three ideal MHD waves. Figure 1 plots the three roots in eqs. 18) 0) versus the propagation angle α for the fixed parameters k ρ s = 0.8 and = 0.5. From the top down, the curves correspond to the fast, and slow modes, respectively. For the sake of comparison, the corresponding ideal MHD solutions are presented as dashed lines in Figure 1. From Figure 1, we see that the fast and modes are considerably modified by the shortwavelength effect in the quasiparallel and quasiperpendicular directions, respectively. The slow mode, however, obviously departs from its ideal MHD version from α = 0 through α = 90 due to the shortwavelength effect. The parallel phase speed of the fast mode increases by a factor of in the quasiparallel direction of α < 0 and that of the mode increases by a factor of in the quasiperpendicular direction of α > 50. For the slow mode, the parallel phase speed decreases by a factor of in the quasiparallel direction of α < 0 and a slightly lower factor of in the quasiperpendicular direction of α > 50 due to the shortwavelength effect. Figure shows the dependence of the dispersion relations for the fast, and slow modes from the top down) on the perpendicular wavenumber k ρ s ) for the quasiparallel α = 15 for the left column) and quasiperpendicular α = 60 for the right column) propagating cases. The fixed parameter = 0.5 has been used and the dashed lines plot the corresponding ideal MHD solutions for the sake of comparison. From Figure, we have found, for all cases, the modification of the dispersion relations to be negligibly small ω /v A k A k ω /v A k ω /v k ρ s =0.8 = α Figure 1 The dispersion relations versus the propagation angle. Panels, from the top down, present the fast, and slow modes, respectively, where the dashed lines plot the corresponding idea MHD solutions, where the parameters k ρ s = 0.8 and = 0.5 have been used.
4 958 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No. 10 A k ω /v A k ω /v A k ω /v.5.0 = b) = 0.5 α = α = a) ω /v A k ω /v A k ω /v A k k ρ s Figure The dispersion relations versus the perpendicular wavenumber. Panels, from the top down, present the fast, and slow modes, respectively, where the dashed lines plot the corresponding idea MHD solutions for the sake of comparison and the left and right columns correspond to the cases of quasiparallel α = 15 ) a) and quasiperpendicular α = 60 ) b) propagations, respectively. k ρ s when k ρ s < 0.1 and to increase quickly with k ρ s when k ρ s > 0.1. This clearly implies that the dispersion modification is caused by the shortwavelength effect in the perpendicular direction. The shortwavelength effect leads to the increase of the parallel phase speed for both the fast and modes, but the decrease for the slow mode. On the other hand, the plasma parameter the ratio of thermal to magnetic pressures) can remarkably influence the dispersion modification as well. Figure 3 shows the dependence of the dispersion relations for the fast, and slow modes from the top down) on the plasma parameter for the quasiparallel α = 15 for the left column) and quasiperpendicular α = 60 for the right column) propagating cases. We have used the fixed perpendicular wavenumber k ρ s = 0.8 and have plotted the corresponding ideal MHD solutions with dashed lines for the sake of comparison. From Figure 3, we find that, for the fast mode, the dispersion modification mainly occurs in the finite regime of 01 < < 1 for the quasiparallel propagating case see the top panel of the left column). For this case, the parallel phase speed is considerably higher than its ideal MHD solution, whereas the modifications are negligibly small for the quasiperpendicular propagating case see the top panel of the right column), as shown in the top panel of Figure 1. On the other hand, for the slow mode, the dispersion modification occurs mainly in the high regime of 0.1 < < 10 for both the quasiparallel and quasiperpendicular propagating cases, in which the parallel phase speed is lower than its ideal MHD solution see the bottom panels in Figure 3). For the mode, however, the matter is more complex. In the low regime of < 01, the parallel phase speed is remarkably lower than its ideal MHD solution, but is higher than its ideal MHD solution in the finite and high regimes of 01 < < 10. For the extremely high regime of > 100, the parallel phase speed of the mode approaches its ideal MHD solution as increases. As shown in Figure 1, the modification in the quasiperpendicular propagation direction is much larger than that in the quasiparallel propagation direction in the finite and high regimes of 01 < < 10. Incidentlally, it is worth noting that, for the quasiparallel propagating case see the left column in Figure 3), both the fast and modes encounter the Landau resonance of electrons near m e /m i < 10 3 due to v A v Te the electron thermal speed), where the flow description is invalid and the kinetic theory becomes necessary.
5 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No A k ω /v A k ω /v A k ω /v 10 a) k ρ s = b) k ρ s =0.8 α = 15 α = ω /v A k ω /v A k ω /v A k Figure 3 The dispersion relations versus plasma beta parameter. Panels, from the top down, present the fast, and slow modes, respectively, where the dashed lines plot the corresponding idea MHD solutions for the sake of comparison and the left and right columns correspond to the cases of quasiparallel α = 15 ) a) and quasiperpendicular α = 60 ) b) propagations, respectively. 3 Lowand quasiperpendicular propagation limits In the low limit of 0, one has approximately, from eq. 14): A K A + k k k, B K A, C = 1 + Q + k λ e k 0. 6) Consequently, the dispersion eq. 13) can be approximated as ) Ω Ω Ω k ) k K A 0. 7) 1 + Q + k λ e Its three roots are Ω S = 0; Ω F = k /k ; Ω A = K A. 8) This indicates that in the low limit the slow mode is ordered out and the fast and modes are reduced to the compressive and the KAW modes, respectively. On the other hand, in the quasiperpendicular propagation limit of k k i.e. k /k 0), one has approximately, from eq. 14): A 1 + Q + k λ e Q + k λ e k, B 1 + Q + k ρ s Q + k λ e C 1 + Q + k λ e k k. 9) Consequently, the dispersion eq. 13) can be approximated as Ω Q + k ρ s Q + k λ e + Ω Q + k λ e + Its two roots, k Ω Q + k λ e 0. 30) 1 + Q + k λ e + k Ω A,S =1 1 + Q + k ρ s Q + k λ e + 1 ± Q + k λ e Q + k ρ s + ), 31),
6 960 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No. 10 are the coupling modes of the and slow modes. In particular, for the low limit of 1, one has Ω A K A; Ω S 1 + Q + k ρ s +. 3) This indicates that the two coupling modes are decoupled into the KAW and ionacoustic modes. The fast mode is ordered out in the quasiperpendicular propagation limit. 4 Summary and conclusion The MHD fast, and slow) waves are intrinsic and ubiquitous fluctuation processes in space and astrophysical plasmas and play an important role in their dynamical coupling and energy transportation. In particular, it has been widely accepted that the dispersive smallscale MHD waves could be responsible for the dissipation of wave energies, as well as particle acceleration and plasma heating, which occur continually in various eruptive phenomena from terrestrial aurora and solar flares, to cosmic rays. The dispersive smallscale wave, called KAW, has been extensively investigated and applied to plasma energiation processes [1 4]. In analogous works, however, little attention has been paid to the fast and slow modes. Recent investigations on the MHD turbulence have proposed that the compressible fluctuations in the fast and slow modes, as well as the KAWs, may need to be taken further into consideration when referring to the steeping of the spectrum at higher wavenumbers [17 0,6]. In this paper, the dispersive MHD waves, with the shortwavelength modification, are selfconsistently revised on the basis of the twofluid model. The dispersion equation, including the shortwavelength effect, and its three roots, are presented as the shortwavelength modification versions of the three ideal MHD fast, and slow) modes. The results show that the fast mode is considerably modified by the shortwavelength effect in the quasiparallel propagation direction and the parallel phase speed increases by a factor of in the quasiparallel propagation direction of α < 0. Moreover, the dispersion modification occurs mainly in the finite regime of 01 < < 1. In contrast to the fast mode, the mode is modified by the shortwavelength effect primarily in the quasiperpendicular propagation direction and the parallel phase speed increases by a factor of in the quasiperpendicular propagation direction of α > 50. In the low regime of < 01, the parallel phase speed is remarkably lower than its ideal MHD solution, whereas the parallel phase speed is higher than its ideal MHD solution in the finite and high regimes of 01 < < 10. Furthermore, in the extremely high regime of > 100, the parallel phase speed of the mode approaches its ideal MHD solution. Different from both the fast and modes, the slow mode clearly departs from its ideal MHD solution between α = 0 and α = 90, due to the shortwavelength effect. The parallel phase speed decreases by a factor of in the quasiparallel propagation direction of α < 0 and a slightly lower factor of in the quasiperpendicular propagation direction of α > 50. Moreover, the dispersion modification occurs predominantly in the high regime of 0.1 < < 10. Finally, our results show further that, in the low limit of 0, the slow mode is ordered out, the fast mode reduces to the compressive mode, and the shear mode leads to KAWs. Conversely, in the quasiperpendicular propagation limit of k k, the fast mode is ordered out and the shear and slow modes become coupled. This work was supported by the National Natural Science Foundation of China , ), and National Basic Research Program of China 011CB81140). 1 Hasegawa A, Uberoi C. The Wave, DOE Critical Review Series Advances in Fusion Science and Engineering, Technical Information Center, U.S. Department of Energy, Washington, DC, 198 Spies G O, Li J. On the kinetic wave. Phys Fluids B, 1990, : Lysak R L, Lotko W. On the kinetic dispersion relation for shear waves. J Geophys Res, 1996, 101: Wu D J, Chao J K. Recent progress in nonlinear kinetic waves. Nonlinear Proc Geoph, 004, 11: Hasegawa A, Chen L. Kinetic processes in plasma heating by resonant mode conversion of wave. Phys Fluids, 1976, 19: Ross D W, Chen G L, Mahajan S M. Kinetic description of wave heating. Phys Fluids, 198, 5: Huang L, Qin X M, Ding N, et al. Heating Finite Beta TokamakPlasmas by Waves. Chin Phys Lett, 1991, 8: Wu D J. Model of nonlinear kinetic waves with dissipation and acceleration of energetic electrons. Phys Rev E, 003, 67: Wu D J. Dissipative solitary kinetic wave and electron acceleration. Phys Plasmas, 003, 10: Wu D J, Chao J K. Auroral electron acceleration by dissipative solitary kinetic waves. Phys Plasmas, 003, 10: Wu D J, Chao J K. Model of auroral electron acceleration by dissipative nonlinear inertial wave. J Geophys Res, 004, 109: A Wu D J, Fang C. Twofluid motion of plasma in waves and the heating of solar coronal loops. ApJ, 1999, 511: Wu D J, Fang C. Coronal plume heating and kinetic dissipation of kinetic waves. ApJ, 003, 596: Wu D J, Fang C. Sunspot chromospheric heating by kinetic waves. ApJ, 007, 659: L181 L Wu D J, Yang L. Anisotropic and massdependent energiation of heavy ions by kinetic. Astron Astrophys, 006, 45: L7 L10 16 Wu D J, Yang L. Nonlinear interaction of minor heavy ions with kinetic waves and their anisotropic energiation in coronal holes. ApJ, 007, 659: Goldreich P, Sridhar S. Toward a theory of interstellar turbulence. : Strong ic turbulence. ApJ, 1995, 438: Goldreich P, Sridhar S. Magnetohydrodynamic turbulence revisited. ApJ, 1997, 485: Galtier S, Naarenko S V, Newell A C, et al. A weak turbulence theory for incompressible magnetohydrodynamics. J Plasma Phys, 000, 63: Galtier S, Chandran B. Extended spectral scaling laws for shear wave turbulence. Phys Plasmas, 006, 13:
7 Chen L, et al. Chinese Sci Bull April 011) Vol. 56 No Heyvaerts J, Priest E R. Coronal heating by phasemixed shear waves. Astron Astrophys, 1983, 117: 0 34 Ofman L, Davila J M. wave heating of coronal holes and the relation to the highspeed solar wind. J Geophys Res, 1995, 100: Lee M A, Roberts B. On the behavior of hydromagnetic surface waves. ApJ, 1986, 301: Hollweg J V. Resonance absorption of magnetohydrodynamic surface waves Physical discussion. ApJ, 1987, 31: Hollweg J V, Yang G. Resonance absorption of compressible magnetohydrodynamic waves at thin surfaces. J Geophys Res, 1988, 93: Howes G G, Cowley S C, Dorland W, et al. A model of turbulence in magnetied plasmas: Implications for the dissipation range in the solar wind. J Geophys Res, 008, 113: A Marson J, Goldreich P. Simulations of incompressible magnetohydrodynamic turbulence. ApJ, 001, 554: Cho J, Laarian A, Vishniac E T. Simulations of magnetohydrodynamic turbulence in a strongly magnetied medium. ApJ, 00, 564: Belcher J W, Davis Jr L. Largeamplitude waves in the interplanetary medium,. J Geophys Res, 1971, 76: Matthaeus W H, Goldstein M L, Roberts D A. Evidence for the presence of quasitwodimensional nearly incompressible fluctuations in the solar wind. J Geophys Res, 1990, 95: Wilkinson P N, Narayan R, Spencer R E. The scatterbroadened image of CYGNUSX3. Mon Not R Astron Soc, 1994, 69: Trotter A S, Moran J M, Rodrigue L F. Anisotropic radio scattering of NGC 6334B. ApJ, 1998, 493: Rickett B J, KedioraChudcer L, Jauncey D L. Interstellar scintillation of the polaried flux density in quasar PKS ApJ, 00, 581: DennettThorpe J, De Bruyn A G. Annual modulation in the scattering of J : Peculiar plasma velocity and anisotropy. Astron Astrophys, 003, 404: Leamon R J, Smith C W, Ness N F, et al. Observational constraints on the dynamics of the interplanetary magnetic field dissipation range. J Geophys Res, 1998, 103: Leamon R J, Smith C W, Ness N F, et al. Damping of oblique kinetic waves as the cause of the interplanetary magnetic field dissipation range. Eos Trans AGU, Spring Meet Suppl, 1998, 79: S7 37 Goert C K. Kinetic waves on auroral field lines. Planet Space Sci, 1984, 3: Hollweg J V. Kinetic wave revisited. J Geophys Res, 1999, 104: Ren Z P, Wan W X, Wei Y, et al. A theoretical model for mid and lowlatitude ionospheric electric fields in realistic geomagnetic fields. Chinese Sci Bull, 008, 53: Zhang Y, Chen J Y, Feng X S. Predicting the shock arrival time using 1DHD solar wind model. Chinese Sci Bull, 010, 55: Yue C, Zong Q G, Wang Y F. Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock. Chinese Sci Bull, 009, 54: Yao L, Liu Z X, Zuo P B, et al. Responses of properties in the plasma sheet and at the geosynchronous orbit to interplanetary shock. Chinese Sci Bull, 009, 54: Sun L P, WU D J, Wang D Y. Suprathermal particle events observed by WIND spacecraft in interplanetary space during and their classification. Sci China Ser ETech Sci, 008, 51: Zhang X G, Pu Z Y, Ma Z W, et al. Roles of initial current carrier in the distribution of fieldaligned current in 3D Hall MHD simulations. Sci China Ser ETech Sci, 008, 51: Li X, Weng C S. D viscous magnetohydrodynamics simulation of plasma armatures with the CE/SE method. Chinese Sci Bull, 009, 54: Lu H Y, Lee C H. Influence of Hall effects on characteristics of magnetohydrodynamic converging channel. Chinese Sci Bull, 010, 55: Lu H Y, Lee C H. Simulation of threedimensional nonideal MHD flow at low magnetic Reynolds number. Sci China Ser ETech Sci, 009, 5: Lu H Y, Lee C H, Dong H T. Characteriation of the threedimensional supersonic flow for the MHD generator. Sci China Ser GPhys Mech Astron, 009, 5: Wu D J. Effects of ion temperature and inertia on kinetic waves. Commun Theor Phys, 003, 39: Open Access This article is distributed under the terms of the Creative Commons Attribution License which permits any use, distribution, and reproduction in any medium, provided the original authors) and source are credited.
Kinetic Alfvén waves in space plasmas
Kinetic Alfvén waves in space plasmas Yuriy Voitenko Belgian Institute for Space Aeronomy, Brussels, Belgium SolarTerrestrial Center of Excellence, Space Pole, Belgium Recent results obtained in collaboration
More informationRole of coherent structures in space plasma turbulence: Filamentation of dispersive Alfvén waves in density channels
Role of coherent structures in space plasma turbulence: Filamentation of dispersive Alfvén waves in density channels T. Passot, P.L. Sulem, D. Borgogno, D. Laveder Observatoire de la Côte d Azur, Nice
More informationSolar Wind Turbulence
Solar Wind Turbulence Presentation to the Solar and Heliospheric Survey Panel W H Matthaeus Bartol Research Institute, University of Delaware 2 June 2001 Overview Context and SH Themes Scientific status
More informationDependence of magnetic field just inside the magnetopause on subsolar standoff distance: Global MHD results
Article SPECIAL ISSUE Basic Plasma Processes in SolarTerrestrial Activities April 2012 Vol.57 No.12: 1438 1442 doi: 10.1007/s1143401149616 SPECIAL TOPICS: Dependence of magnetic field just inside the
More informationThe evolution of solar wind turbulence at kinetic scales
International Association of Geomagnetism and Aeronomy (IAGA) 2 nd Symposium: Solar Wind Space Environment Interaction c 2010 Cairo University Press December 4 th 8 th, 2009, Cairo, Egypt L.Damé & A.Hady
More informationSpace Physics. An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres. MayBritt Kallenrode. Springer
MayBritt Kallenrode Space Physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres With 170 Figures, 9 Tables, Numerous Exercises and Problems Springer Contents 1. Introduction
More information3D hybridkinetic turbulence and phasespace cascades
3D hybridkinetic turbulence and phasespace cascades ( in a β = 1 plasma ) Silvio Sergio Cerri Department of Astrophysical Sciences, Princeton University, USA 11th Plasma Kinetics Working Meeting WPI
More informationKinetic Turbulence in the Terrestrial Magnetosheath: Cluster. Observations
1 2 Kinetic Turbulence in the Terrestrial Magnetosheath: Cluster Observations 3 4 5 S. Y. Huang 1, F. Sahraoui 2, X. H. Deng 1,3, J. S. He 4, Z. G. Yuan 1, M. Zhou 3, Y. Pang 3, H. S. Fu 5 6 1 School of
More informationGreg Hammett Imperial College, London & Princeton Plasma Physics Lab With major contributions from:
Greg Hammett Imperial College, London & Princeton Plasma Physics Lab With major contributions from: Steve Cowley (Imperial College) Bill Dorland (Imperial College) Eliot Quataert (Berkeley) LMS Durham
More information20. Alfven waves. ([3], p ; [1], p ; Chen, Sec.4.18, p ) We have considered two types of waves in plasma:
Phys780: Plasma Physics Lecture 20. Alfven Waves. 1 20. Alfven waves ([3], p.233239; [1], p.202237; Chen, Sec.4.18, p.136144) We have considered two types of waves in plasma: 1. electrostatic Langmuir
More informationMagnetohydrodynamic Waves
Magnetohydrodynamic Waves Nick Murphy HarvardSmithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics February 17, 2016 These slides are largely based off of 4.5 and 4.8 of The Physics of
More informationWaves in plasma. Denis Gialis
Waves in plasma Denis Gialis This is a short introduction on waves in a nonrelativistic plasma. We will consider a plasma of electrons and protons which is fully ionized, nonrelativistic and homogeneous.
More informationHeating of Test Particles in Numerical Simulations of MHD Turbulence and the Solar Wind
Heating of Test Particles in Numerical Simulations of MHD Turbulence and the Solar Wind Ian Parrish UC Berkeley Collaborators: Rémi Lehe (ENS), Eliot Quataert (UCB) Einstein Fellows Symposium October 27,
More informationPlasma Physics for Astrophysics
 ' ' * ' Plasma Physics for Astrophysics RUSSELL M. KULSRUD PRINCETON UNIVERSITY E;RESS '. ' PRINCETON AND OXFORD,, ', V. List of Figures Foreword by John N. Bahcall Preface Chapter 1. Introduction 1
More informationMHD Modes of Solar Plasma Structures
PX420 Solar MHD 20132014 MHD Modes of Solar Plasma Structures Centre for Fusion, Space & Astrophysics Wave and oscillatory processes in the solar corona: Possible relevance to coronal heating and solar
More informationPLASMA ASTROPHYSICS. ElisaBete M. de Gouveia Dal Pino IAGUSP. NOTES: (references therein)
PLASMA ASTROPHYSICS ElisaBete M. de Gouveia Dal Pino IAGUSP NOTES:http://www.astro.iag.usp.br/~dalpino (references therein) ICTPSAIFR, October 718, 2013 Contents What is plasma? Why plasmas in astrophysics?
More informationFundamentals of Turbulence
Fundamentals of Turbulence Stanislav Boldyrev (University of Wisconsin  Madison) Center for Magnetic SelfOrganization in Laboratory and Astrophysical Plasmas What is turbulence? No exact definition.
More informationDispersive Media, Lecture 7  Thomas Johnson 1. Waves in plasmas. T. Johnson
20170214 Dispersive Media, Lecture 7  Thomas Johnson 1 Waves in plasmas T. Johnson Introduction to plasmas as a coupled system MagnetoHydro Dynamics, MHD Plasmas without magnetic fields Cold plasmas
More informationSimulation study on the nonlinear EMIC waves
SH21B2210 Simulation study on the nonlinear EMIC waves Kicheol Rha 1*, ChangMo Ryu 1 and Peter H Yoon 2 * lancelot@postech.ac.kr 1 Department of Physics, Pohang University of Science and Technology,
More informationHeating of ions by lowfrequency Alfven waves
PHYSICS OF PLASMAS 14, 433 7 Heating of ions by lowfrequency Alfven waves Quanming Lu School of Earth and Space Sciences, University of Science and Technology of China, Hefei 36, People s Republic of
More informationMacroscopic plasma description
Macroscopic plasma description Macroscopic plasma theories are fluid theories at different levels single fluid (magnetohydrodynamics MHD) twofluid (multifluid, separate equations for electron and ion
More informationMHD turbulence in the solar corona and solar wind
MHD turbulence in the solar corona and solar wind Pablo Dmitruk Departamento de Física, FCEN, Universidad de Buenos Aires Motivations The role of MHD turbulence in several phenomena in space and solar
More informationCoronal Heating Problem
PHY 690C Project Report Coronal Heating Problem by Mani Chandra, Arnab Dhabal and Raziman T V (Y6233) (Y7081) (Y7355) Mentor: Dr. M.K. Verma 1 Contents 1 Introduction 3 2 The Coronal Heating Problem 4
More informationA Model for Periodic Nonlinear Electric Field Structures in Space Plasmas
Commun. Theor. Phys. (Beijing, China) 52 (2009) pp. 149 154 c Chinese Physical Society and IOP Publishing Ltd Vol. 52, No. 1, July 15, 2009 A Model for Periodic Nonlinear Electric Field Structures in Space
More informationPlasma waves in the fluid picture I
Plasma waves in the fluid picture I Langmuir oscillations and waves Ionacoustic waves Debye length Ordinary electromagnetic waves General wave equation General dispersion equation Dielectric response
More informationTwodimensional hybrid simulations of filamentary structures. and kinetic slow waves downstream of a quasiparallel shock
Twodimensional hybrid simulations of filamentary structures and kinetic slow waves downstream of a quasiparallel shock Yufei Hao 1,2,3, Quanming Lu 1,3, Xinliang Gao 1,3, Huanyu Wang 1,3, Dejin Wu 4,
More informationSolar Wind Turbulent Heating by Interstellar Pickup Protons: 2Component Model
Solar Wind Turbulent Heating by Interstellar Pickup Protons: 2Component Model Philip A. Isenberg a, Sean Oughton b, Charles W. Smith a and William H. Matthaeus c a Inst. for Study of Earth, Oceans and
More informationCoronal heating and energetics
Coronal heating and energetics Magnetic structures in the solar corona Coronal heating, what does it mean? Flares and coronal cooling Observations of MHD waves in loops Dissipation processes in the corona
More informationSpace Physics. ELECE4520 (5 cr) Teacher: Esa Kallio Assistant: Markku Alho and Riku Järvinen. Aalto University School of Electrical Engineering
Space Physics ELECE4520 (5 cr) Teacher: Esa Kallio Assistant: Markku Alho and Riku Järvinen Aalto University School of Electrical Engineering The 6 th week: topics Last week: Examples of waves MHD: Examples
More informationPROBLEM 1 (15 points) In a Cartesian coordinate system, assume the magnetic flux density
PROBLEM 1 (15 points) In a Cartesian coordinate system, assume the magnetic flux density varies as ( ) where is a constant, is the unit vector in x direction. a) Sketch the magnetic flux density and the
More informationWaveparticle interactions in dispersive shear Alfvèn waves
Waveparticle interactions in dispersive shear Alfvèn waves R. Rankin and C. E. J. Watt Department of Physics, University of Alberta, Edmonton, Canada. Outline Auroral electron acceleration in short parallel
More informationReduced MHD. Nick Murphy. HarvardSmithsonian Center for Astrophysics. Astronomy 253: Plasma Astrophysics. February 19, 2014
Reduced MHD Nick Murphy HarvardSmithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics February 19, 2014 These lecture notes are largely based on Lectures in Magnetohydrodynamics by Dalton
More informationHeating and current drive: Radio Frequency
Heating and current drive: Radio Frequency Dr Ben Dudson Department of Physics, University of York Heslington, York YO10 5DD, UK 13 th February 2012 Dr Ben Dudson Magnetic Confinement Fusion (1 of 26)
More information2/8/16 Dispersive Media, Lecture 5  Thomas Johnson 1. Waves in plasmas. T. Johnson
2/8/16 Dispersive Media, Lecture 5  Thomas Johnson 1 Waves in plasmas T. Johnson Introduction to plasma physics MagnetoHydro Dynamics, MHD Plasmas without magnetic fields Cold plasmas Transverse waves
More informationKinetic and Small Scale Solar Wind Physics
Chapter 11 Kinetic and Small Scale Solar Wind Physics Thus far the origin, evolution, and large scale characteristics of the solar wind have been addressed using MHD theory and observations. In this lecture
More informationEffect of current sheets on the power spectrum of the solar wind magnetic field using a cell model
Available online at www.sciencedirect.com Advances in Space Research 49 (2012) 1327 1332 www.elsevier.com/locate/asr Effect of current sheets on the power spectrum of the solar wind magnetic field using
More informationSW103: Lecture 2. Magnetohydrodynamics and MHD models
SW103: Lecture 2 Magnetohydrodynamics and MHD models Scale sizes in the Solar Terrestrial System: or why we use MagnetoHydroDynamics SunEarth distance = 1 Astronomical Unit (AU) 200 R Sun 20,000 R E 1
More informationTurbulent dissipation in the solar wind and corona
Turbulent dissipation in the solar wind and corona W. H. Matthaeus, P. Dmitruk, S. Oughton and D. Mullan Bartol Research Institute, University of Delaware, Newark, DE 19716 USA Department of Mathematics,
More informationTHE PHYSICS OF PARTICLE ACCELERATION BY COLLISIONLESS SHOCKS
THE PHYSICS OF PARTICLE ACCELERATION BY COLLISIONLESS SHOCKS Joe Giacalone Lunary & Planetary Laboratory, University of Arizona, Tucson, AZ, 8572, USA ABSTRACT Using analytic theory, testparticle simulations,
More informationTURBULENT TRANSPORT THEORY
ASDEX Upgrade MaxPlanckInstitut für Plasmaphysik TURBULENT TRANSPORT THEORY C. Angioni GYRO, J. Candy and R.E. Waltz, GA The problem of Transport Transport is the physics subject which studies the physical
More informationICMs and the IPM: Birds of a Feather?
ICMs and the IPM: Birds of a Feather? Tom Jones University of Minnesota 11 November, 2014 KAW8: Astrophysics of HighBeta Plasma in the Universe 1 Outline: ICM plasma is the dominant baryon component in
More informationMagnetohydrodynamic Turbulence
Magnetohydrodynamic Turbulence Stanislav Boldyrev (UWMadison) Jean Carlos Perez (U. New Hampshire), Fausto Cattaneo (U. Chicago), Joanne Mason (U. Exeter, UK) Vladimir Zhdankin (UWMadison) Konstantinos
More informationScattering of ECRF waves by edge density fluctuations and blobs
PSFC/JA147 Scattering of ECRF waves by edge density fluctuations and blobs A. K. Ram and K. Hizanidis a June 2014 Plasma Science and Fusion Center, Massachusetts Institute of Technology Cambridge, MA
More informationHybrid simulation of ion cyclotron resonance in the solar wind: Evolution of velocity distribution functions
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 110,, doi:10.1029/2005ja011030, 2005 Hybrid simulation of ion cyclotron resonance in the solar wind: Evolution of velocity distribution functions Xing Li Institute
More informationSpacecraft observations of solar wind turbulence: an overview
INSTITUTE OF PHYSICS PUBLISHING Plasma Phys. Control. Fusion 47 (2005) B703 B717 PLASMA PHYSICS AND CONTROLLED FUSION doi:10.1088/07413335/47/12b/s52 Spacecraft observations of solar wind turbulence:
More informationThe O + Ion Flux in the Martian Magnetosphere and Martian Intrinsic Moment
Chin. J. Astron. Astrophys. Vol. 1, No. 2, (2001 185 189 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn Chinese Journal of Astronomy and Astrophysics The O + Ion Flux in the Martian Magnetosphere and
More informationSmall scale solar wind turbulence: Recent observations and theoretical modeling
Small scale solar wind turbulence: Recent observations and theoretical modeling F. Sahraoui 1,2 & M. Goldstein 1 1 NASA/GSFC, Greenbelt, USA 2 LPP, CNRSEcole Polytechnique, Vélizy, France Outline Motivations
More informationSimulation Study of HighFrequency Magnetosonic Waves Excited by Energetic Ions in Association with Ion Cyclotron Emission )
Simulation Study of HighFrequency Magnetosonic Waves Excited by Energetic Ions in Association with Ion Cyclotron Emission ) Mieko TOIDA 1),KenjiSAITO 1), Hiroe IGAMI 1), Tsuyoshi AKIYAMA 1,2), Shuji KAMIO
More informationNonlinear processes associated with Alfvén waves in a laboratory plasma
Nonlinear processes associated with Alfvén waves in a laboratory plasma Troy Carter Dept. Physics and Astronomy and Center for Multiscale Plasma Dynamics, UCLA acknowledgements: Brian Brugman, David Auerbach,
More informationMagnetohydrodynamic Turbulence: solar wind and numerical simulations
Magnetohydrodynamic Turbulence: solar wind and numerical simulations Stanislav Boldyrev (UWMadison) Jean Carlos Perez (U. New Hampshire) Fausto Cattaneo (U. Chicago) Joanne Mason (U. Exeter, UK) Vladimir
More informationJournal of Geophysical Research: Space Physics
RESEARCH ARTICLE Special Section: Nature of Turbulence, Dissipation, and Heating in Space Plasmas: From Alfven Waves to Kinetic Alfven Waves Key Points: Mechanisms to produce kinetic Alfvén waves in pressurebalance
More informationCoronal Heating versus Solar Wind Acceleration
SOHO 15: Coronal Heating, 6 9 September 2004, University of St. Andrews, Scotland Coronal Heating versus Solar Wind Acceleration Steven R. Cranmer HarvardSmithsonian Center for Astrophysics, Cambridge,
More informationHigh energy particles from the Sun. Arto Sandroos SunEarth connections
High energy particles from the Sun Arto Sandroos SunEarth connections 25.1.2006 Background In addition to the solar wind, there are also particles with higher energies emerging from the Sun. First observations
More informationSOLAR WIND ION AND ELECTRON DISTRIBUTION FUNCTIONS AND THE TRANSITION FROM FLUID TO KINETIC BEHAVIOR
SOLAR WIND ION AND ELECTRON DISTRIBUTION FUNCTIONS AND THE TRANSITION FROM FLUID TO KINETIC BEHAVIOR JUSTIN C. KASPER HARVARDSMITHSONIAN CENTER FOR ASTROPHYSICS GYPW01, Isaac Newton Institute, July 2010
More informationIdeal Magnetohydrodynamics (MHD)
Ideal Magnetohydrodynamics (MHD) Nick Murphy HarvardSmithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics February 1, 2016 These lecture notes are largely based on Lectures in Magnetohydrodynamics
More informationFluid modeling of anisotropic heating and microinstabilities
Fluid modeling of anisotropic heating and microinstabilities in space plasmas Thierry Passot UNS, CNRS, Observatoire de la Côte d Azur, Nice, France Collaborators: D. Laveder, L. Marradi, and P.L. Sulem
More informationSpace Plasma Physics Thomas Wiegelmann, 2012
Space Plasma Physics Thomas Wiegelmann, 2012 1. Basic Plasma Physics concepts 2. Overview about solar system plasmas Plasma Models 3. Single particle motion, Test particle model 4. Statistic description
More informationAnisotropic electron distribution functions and the transition between the Weibel and the whistler instabilities
Anisotropic electron distribution functions and the transition between the Weibel and the whistler instabilities F. Pegoraro, L. Palodhi, F. Califano 5 th INTERNATIONAL CONFERENCE ON THE FRONTIERS OF PLASMA
More informationThe Physics of Fluids and Plasmas
The Physics of Fluids and Plasmas An Introduction for Astrophysicists ARNAB RAI CHOUDHURI CAMBRIDGE UNIVERSITY PRESS Preface Acknowledgements xiii xvii Introduction 1 1. 3 1.1 Fluids and plasmas in the
More informationStability of a plasma confined in a dipole field
PHYSICS OF PLASMAS VOLUME 5, NUMBER 10 OCTOBER 1998 Stability of a plasma confined in a dipole field Plasma Fusion Center, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139 Received
More informationA Comparison between the Twofluid Plasma Model and HallMHD for Captured Physics and Computational Effort 1
A Comparison between the Twofluid Plasma Model and HallMHD for Captured Physics and Computational Effort 1 B. Srinivasan 2, U. Shumlak Aerospace and Energetics Research Program University of Washington,
More informationNONLINEAR MHD WAVES THE INTERESTING INFLUENCE OF FIREHOSE AND MIRROR IN ASTROPHYSICAL PLASMAS. Jono Squire (Caltech) UCLA April 2017
NONLINEAR MHD WAVES THE INTERESTING INFLUENCE OF FIREHOSE AND MIRROR IN ASTROPHYSICAL PLASMAS Jono Squire (Caltech) UCLA April 2017 Along with: E. Quataert, A. Schekochihin, M. Kunz, S. Bale, C. Chen,
More informationELECTROSTATIC IONCYCLOTRON WAVES DRIVEN BY PARALLEL VELOCITY SHEAR
1 ELECTROSTATIC IONCYCLOTRON WAVES DRIVEN BY PARALLEL VELOCITY SHEAR R. L. Merlino Department of Physics and Astronomy University of Iowa Iowa City, IA 52242 December 21, 2001 ABSTRACT Using a fluid treatment,
More informationThe Physics of Collisionless Accretion Flows. Eliot Quataert (UC Berkeley)
The Physics of Collisionless Accretion Flows Eliot Quataert (UC Berkeley) Accretion Disks: Physical Picture Simple Consequences of Mass, Momentum, & Energy Conservation Matter Inspirals on Approximately
More informationCoronal heating and energetics
Coronal heating and energetics Magnetic structures in the solar corona Coronal heating, what does it mean? Flares and coronal cooling Observations of MHD waves in loops Dissipation processes in the corona
More informationChapter 1. Introduction to Nonlinear Space Plasma Physics
Chapter 1. Introduction to Nonlinear Space Plasma Physics The goal of this course, Nonlinear Space Plasma Physics, is to explore the formation, evolution, propagation, and characteristics of the large
More informationEnergy Analysis During the Collision of Two Successive CMEs
Numerical Modeling of Space Plasma Flows: ASTRONUM2013 ASP Conference Series, Vol. 488 N.V.Pogorelov, E.Audit,and G.P.Zank,eds. c 2014 Astronomical Society of the Pacific Energy Analysis During the Collision
More informationMagnetic Reconnection: explosions in space and astrophysical plasma. J. F. Drake University of Maryland
Magnetic Reconnection: explosions in space and astrophysical plasma J. F. Drake University of Maryland Magnetic Energy Dissipation in the Universe The conversion of magnetic energy to heat and high speed
More informationLinear and nonlinear evolution of the gyroresonance instability in Cosmic Rays
Linear and nonlinear evolution of the gyroresonance instability in Cosmic Rays DESY Summer Student Programme, 2016 Olga Lebiga Taras Shevchenko National University of Kyiv, Ukraine Supervisors Reinaldo
More informationAcceleration of energetic particles by compressible plasma waves of arbitrary scale sizes DOI: /ICRC2011/V10/0907
3ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING Acceleration of energetic particles by compressible plasma s of arbitrary scale sizes MING ZHANG Department of Physics and Space Sciences, Florida Institute
More informationExtended Coronal Heating and Solar Wind Acceleration over the Solar Cycle
Extended Coronal Heating and Solar Wind Acceleration over the Solar Cycle S. R. Cranmer, J. L. Kohl, M. P. Miralles, & A. A. van Ballegooijen HarvardSmithsonian Center for Astrophysics Extended Coronal
More informationAlfvénic Turbulence in the Fast Solar Wind: from cradle to grave
Alfvénic Turbulence in the Fast Solar Wind: from cradle to grave, A. A. van Ballegooijen, and the UVCS/SOHO Team HarvardSmithsonian Center for Astrophysics Alfvénic Turbulence in the Fast Solar Wind:
More informationMesoscale Variations in the Heliospheric Magnetic Field and their Consequences in the Outer Heliosphere
Mesoscale Variations in the Heliospheric Magnetic Field and their Consequences in the Outer Heliosphere L. A. Fisk Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor,
More informationMagnetohydrodynamic waves in a plasma
Department of Physics Seminar 1b Magnetohydrodynamic waves in a plasma Author: Janez Kokalj Advisor: prof. dr. Tomaž Gyergyek Petelinje, April 2016 Abstract Plasma can sustain different wave phenomena.
More informationEarth s Bow Shock and Magnetosheath
Chapter 12 Earth s Bow Shock and Magnetosheath Aims and Learning Outcomes The Aim of this Chapter is to explore in more detail the physics of fast mode shocks and to introduce the physics of planetary
More informationIntroduction to Magnetohydrodynamics (MHD)
Introduction to Magnetohydrodynamics (MHD) Tony Arber University of Warwick 4th SOLARNET Summer School on Solar MHD and Reconnection Aim Derivation of MHD equations from conservation laws Quasineutrality
More informationElectromagneic Waves in a non Maxwellian Dusty Plasma
Electromagneic Waves in a non Maxwellian Dusty Plasma Nazish Rubab PhD student, KF University Graz IWFOEAW Graz 26 January, 2011 Layout Dusty Plasma NonMaxwellian Plasma Kinetic Alfven Waves Instability
More informationIncompressible MHD simulations
Incompressible MHD simulations Felix Spanier 1 Lehrstuhl für Astronomie Universität Würzburg Simulation methods in astrophysics Felix Spanier (Uni Würzburg) Simulation methods in astrophysics 1 / 20 Outline
More informationMHD turbulence in the solar corona and solar wind
MHD turbulence in the solar corona and solar wind Pablo Dmitruk Departamento de Física, FCEN, Universidad de Buenos Aires Turbulence, magnetic reconnection, particle acceleration Understand the mechanisms
More informationTurbulent Origins of the Sun s Hot Corona and the Solar Wind
Turbulent Origins of the Sun s Hot Corona and the Solar Wind Steven R. Cranmer HarvardSmithsonian Center for Astrophysics Turbulent Origins of the Sun s Hot Corona and the Solar Wind Outline: 1. Solar
More informationSuperdiffusive and subdiffusive transport of energetic particles in astrophysical plasmas: numerical simulations and experimental evidence
Superdiffusive and subdiffusive transport of energetic particles in astrophysical plasmas: numerical simulations and experimental evidence Gaetano Zimbardo S. Perri, P. Pommois, and P. Veltri Universita
More informationPlasma Processes. m v = ee. (2)
Plasma Processes In the preceding few lectures, we ve focused on specific microphysical processes. In doing so, we have ignored the effect of other matter. In fact, we ve implicitly or explicitly assumed
More informationTHEORETICAL RESEARCH ON SOLAR WIND TURBULENCE
THEORETICAL RESEARCH ON SOLAR WIND TURBULENCE A White Paper Submitted to the NRC Decadal Survey of Solar and Space Physics Benjamin D. G. Chandran, Eliot Quataert, Jean Perez, Aveek Sarkar, Steve Cranmer,
More informationProf. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit
Prof. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit Rough breakdown of MHD shocks Jump conditions: flux in = flux out mass flux: ρv n magnetic flux: B n Normal momentum flux: ρv n
More informationLet s consider nonrelativistic electrons. A given electron follows Newton s law. m v = ee. (2)
Plasma Processes Initial questions: We see all objects through a medium, which could be interplanetary, interstellar, or intergalactic. How does this medium affect photons? What information can we obtain?
More informationIon vs. Electron Heating by Plasma Turbulence
WPI, Vienna 30 July 2018 Ion vs. Electron Heating by Plasma Turbulence (an accretiondisc problem that opened the plasmagates ) Yohei Kawazura, Michael Barnes & Alex Schekochihin (Oxford) with thanks to
More informationSunEarth Connection Missions
ACE (1997 ) Cosmic and Heliospheric Study of the physics and chemistry Advanced Composition Explorer Learning Center of the solar corona, the solar wind, http://helios.gsfc.nasa.gov/ace/ http://helios.gsfc.nasa.gov
More informationIntroduction to Plasma Physics
Introduction to Plasma Physics Hartmut Zohm MaxPlanckInstitut für Plasmaphysik 85748 Garching DPG Advanced Physics School The Physics of ITER Bad Honnef, 22.09.2014 A simplistic view on a Fusion Power
More informationVerification of ShortTerm Predictions of Solar Soft Xray Bursts for the Maximum Phase ( ) of Solar Cycle 23
Chin. J. Astron. Astrophys. Vol. 3 (2003), No. 6, 563 568 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics Verification of ShortTerm Predictions of Solar
More informationMagnetic Reconnection in Laboratory, Astrophysical, and Space Plasmas
Magnetic Reconnection in Laboratory, Astrophysical, and Space Plasmas Nick Murphy HarvardSmithsonian Center for Astrophysics namurphy@cfa.harvard.edu http://www.cfa.harvard.edu/ namurphy/ November 18,
More information1 TH/P843 Role of Impurity Cyclotron Damping in Ion Heating and RFP Turbulence
1 Role of Impurity Cyclotron Damping in Ion Heating and RFP Turbulence P.W. Terry, V. Tangri, J.S. Sarff, G. Fiksel, A.F. Almagri, Y. Ren, and S.C. Prager Department of Physics, University of WisconsinMadison,
More informationObservations of counterpropagating Alfvénic and compressive fluctuations in the chromosphere
RAA 2014 Vol. 14 No. 3, 299 310 doi: 10.1088/1674 4527/14/3/004 http://www.raajournal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Observations of counterpropagating Alfvénic
More informationForced hybridkinetic turbulence in 2D3V
Forced hybridkinetic turbulence in 2D3V Silvio Sergio Cerri1,2 1 In collaboration with: 3 F. Califano, F. Rincon, F. Jenko4, D. Told4 1 Physics Department E. Fermi, University of Pisa, Italy fu r Plasmaphysik,
More informationParticle in cell simulations of circularly polarised Alfvén wave phase mixing: A new mechanism for electron acceleration in collisionless plasmas
Particle in cell simulations of circularly polarised Alfvén wave phase mixing: A new mechanism for electron acceleration in collisionless plasmas Tsiklauri, D, Sakai, JI and Saito, S http://dx.doi.org/10.1051/0004
More informationPrediction of solar activity cycles by assimilating sunspot data into a dynamo model
Solar and Stellar Variability: Impact on Earth and Planets Proceedings IAU Symposium No. 264, 2009 A. G. Kosovichev, A. H. Andrei & J.P. Rozelot, eds. c International Astronomical Union 2010 doi:10.1017/s1743921309992638
More informationAnalysis of Jeans Instability of PartiallyIonized. Molecular Cloud under Influence of Radiative. Effect and Electron Inertia
Adv. Studies Theor. Phys., Vol. 5, 2011, no. 16, 755764 Analysis of Jeans Instability of PartiallyIonized Molecular Cloud under Influence of Radiative Effect and Electron Inertia B. K. Dangarh Department
More informationCollisions and transport phenomena
Collisions and transport phenomena Collisions in partly and fully ionized plasmas Typical collision parameters Conductivity and transport coefficients Conductivity tensor Formation of the ionosphere and
More informationA ThreeFluid Approach to Model Coupling of Solar WindMagnetosphereIonosphere Thermosphere
A ThreeFluid Approach to Model Coupling of Solar WindMagnetosphereIonosphere Thermosphere P. Song Center for Atmospheric Research University of Massachusetts Lowell V. M. Vasyliūnas MaxPlanckInstitut
More informationUNCONDITIONAL STABILITY OF A PARTITIONED IMEX METHOD FOR MAGNETOHYDRODYNAMIC FLOWS
UNCONDITIONAL STABILITY OF A PARTITIONED IMEX METHOD FOR MAGNETOHYDRODYNAMIC FLOWS CATALIN TRENCHEA Key words. magnetohydrodynamics, partitioned methods, IMEX methods, stability, Elsässer variables. Abstract.
More informationarxiv: v2 [astroph.sr] 3 Aug 2010
Correlations between the proton temperature anisotropy and transverse highfrequency waves in the solar wind Sofiane Bourouaine 1, Eckart Marsch 1 and Fritz M. Neubauer 2 arxiv:1003.2299v2 [astroph.sr]
More information