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Journal articles on the topic 'Alfven- Kinetic waves'

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Published: 6 September 2023

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1

Kar, C., S. K. Majumdar, and A. N. Sekar Iyengar. "Stabilization of collisional drift waves by kinetic Alfvén waves." Journal of Plasma Physics 47, no. 2 (1992): 249–60. http://dx.doi.org/10.1017/s002237780002420x.

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We have investigated a mode-coupling mechanism between kinetic Alfvén waves and a collisional drift wave in an inhomogeneous cylindrical plasma. Drift waves satisfying the condition k⊥D > 1/r0 (where r0 is the radius of the plasma cylinder) are stabilized by the low-frequency ponderomotive force generated by the kinetic Alfvén waves. For typical plasma parameters and a moderate level of Alfven-wave intensity the stabilization factor is comparable to the destabilization mechanism due to collisions.

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2

Liu, W. W. "Chaos driven by kinetic Alfven waves." Geophysical Research Letters 18, no. 8 (1991): 1611–14. http://dx.doi.org/10.1029/91gl01779.

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3

NAKAMURA, Tadas K. ""Kinetic" Alfven Waves and Parallel Electric Fields." Journal of Plasma and Fusion Research 78, no. 10 (2002): 1043–48. http://dx.doi.org/10.1585/jspf.78.1043.

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4

Wu, D. J., and C. Fang. "Coronal Plume Heating and Kinetic Dissipation of Kinetic Alfven Waves." Astrophysical Journal 596, no. 1 (2003): 656–62. http://dx.doi.org/10.1086/377599.

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5

Voitenko, Yu, M. Goossens, A. K. Yukhimuk, and A. D. Voitsekhovska. "Alfven waves in space plasmas: dispersive and kinetic effects." Kosmìčna nauka ì tehnologìâ 7, no. 2s (2001): 67–73. http://dx.doi.org/10.15407/knit2001.02s.067.

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6

Yukhimuk, A. K., V. N. Fedun, A. D. Voitsekhovska, and O. K. Cheremnykh. "Generation of kinetic Alfven waves in a cosmic plasma." Kosmìčna nauka ì tehnologìâ 8, no. 2s (2002): 228–36. http://dx.doi.org/10.15407/knit2002.02s.228.

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7

Agarwal, P., P. Varma, and M. S. Tiwari. "Study of inertial kinetic Alfven waves around cusp region." Planetary and Space Science 59, no. 4 (2011): 306–11. http://dx.doi.org/10.1016/j.pss.2010.11.006.

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8

Venugopal, Chandu, R. Jayapal, G. Sreekala, Blesson Jose, E. Savithri Devi, and S. Antony. "Dispersion characteristics of kinetic Alfven waves in a multi-ion plasma." Physica Scripta 89, no. 6 (2014): 065604. http://dx.doi.org/10.1088/0031-8949/89/6/065604.

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9

Rubab, N., and G. Jaffer. "Excitation of dust kinetic Alfven waves by semi-relativistic ion beams." Physics of Plasmas 23, no. 5 (2016): 053701. http://dx.doi.org/10.1063/1.4948490.

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10

Shrivastava, J., and G. Shrivastava. "Kinetic Alfven waves in plasma sheet boundary layer—particle aspect analysis." Planetary and Space Science 56, no. 9 (2008): 1214–25. http://dx.doi.org/10.1016/j.pss.2008.04.001.

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11

Kirchner, T. M., and J. Büchner. "On electron acceleration in extended radio sources by kinetic Alfven waves." Advances in Space Research 10, no. 9 (1990): 39–42. http://dx.doi.org/10.1016/0273-1177(90)90206-f.

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12

Panwar, A., C. M. Ryu, and A. S. Bains. "Kinetic Alfven solitary waves in a magnetized plasma with superthermal electrons." Physics of Plasmas 22, no. 9 (2015): 092130. http://dx.doi.org/10.1063/1.4931993.

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13

Rowe, GW. "Collisionless Damping of Fast and Ion?Cyclotron Surface Waves." Australian Journal of Physics 46, no. 2 (1993): 271. http://dx.doi.org/10.1071/ph930271.

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A recently developed general kinetic theory of surface waves is used to calculate the collisionless damping of low frequency fast and ion-cyclotron surface waves on a magnetised plasma-vacuum interface. In particular, the possibility of Cherenkov (Landau and transit-time magnetic) absorption by electrons is accounted for, assuming a bi-Maxwellian distribution of electrons in velocity space. It is shown that in general the surface waves are damped via mode conversion to a short-wavelength mode, such as the kinetic Alfven wave, which is subsequently Landau absorbed within the plasma. For high temperatures this short-wavelength mode can also be radiated into the plasma without being completely absorbed. It is also shown that the related ion-sound surface wave mode and instability identified by Alexandrov et al. (1984) are unphysical, and are the result of neglecting the gas pressure in the first-order magnetic field boundary condition.

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14

Samuel, George, Devi E. Savithri, and Venugopal Chandu. "Kinetic Alfven Waves Excited by Cometary Newborn Ions with Large Perpendicular Energies." Plasma Science and Technology 13, no. 2 (2011): 135–39. http://dx.doi.org/10.1088/1009-0630/13/2/02.

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15

Sadiq, Nauman, and Mushtaq Ahmad. "Kinetic Alfven waves in dense quantum plasmas with effect of spin magnetization." Plasma Research Express 1, no. 2 (2019): 025007. http://dx.doi.org/10.1088/2516-1067/ab168f.

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16

Adnan, Muhammad, Sahahzad Mahmood, Anisa Qamar, and Mouloud Tribeche. "Small amplitude Kinetic Alfven waves in a superthermal electron–positron–ion plasma." Advances in Space Research 58, no. 9 (2016): 1746–54. http://dx.doi.org/10.1016/j.asr.2016.07.009.

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17

Artemyev, A. V., R. Rankin, and M. Blanco. "Electron trapping and acceleration by kinetic Alfven waves in the inner magnetosphere." Journal of Geophysical Research: Space Physics 120, no. 12 (2015): 10,305–10,316. http://dx.doi.org/10.1002/2015ja021781.

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18

Shrivastava, G., and J. Shrivastava. "Electron Beam Effects on Kinetic Alfven Waves in the Plasma Sheet Boundary Layer." OALib 01, no. 07 (2014): 1–9. http://dx.doi.org/10.4236/oalib.1100518.

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19

Yukhimuk, A. K., V. N. Fedun, V. A. Yukhimuk, and V. N. Ivchenko. "Parametric excitation of upper hybrid and kinetic alfven waves in a magnetized plasma." Kosmìčna nauka ì tehnologìâ 4, no. 1 (1998): 108–12. http://dx.doi.org/10.15407/knit1998.01.108.

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20

Kryshtal, A. N., and S. V. Gerasimenko. "The generation of kinetic alfven waves in the loop's plasma in active region." Kosmìčna nauka ì tehnologìâ 10, no. 4 (2004): 81–91. http://dx.doi.org/10.15407/knit2004.04.081.

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21

Amagishi, Y. "Laboratory experiment on kinetic Alfven waves in connection with phenomena in space plasmas." IEEE Transactions on Plasma Science 20, no. 6 (1992): 622–25. http://dx.doi.org/10.1109/27.199502.

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22

Bashir, M. F., Lunjin Chen, and Raluca Ilie. "Theoretical Prediction of Asymmetric Instability of Drift Kinetic Alfven Waves in Anisotropic Plasmas." Journal of Geophysical Research: Space Physics 124, no. 6 (2019): 4414–23. http://dx.doi.org/10.1029/2019ja026615.

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23

Sabeen, A., H. A. Shah, W. Masood, and M. N. S. Qureshi. "Finite amplitude solitary structures of coupled kinetic Alfven-acoustic waves in dense plasmas." Astrophysics and Space Science 355, no. 2 (2014): 225–32. http://dx.doi.org/10.1007/s10509-014-2169-3.

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24

Sabeen, A., W. Masood, M. N. S. Qureshi, and H. A. Shah. "Nonlinear coupling of kinetic Alfven waves with acoustic waves in a self-gravitating dusty plasma with adiabatic trapping." Physics of Plasmas 24, no. 7 (2017): 073704. http://dx.doi.org/10.1063/1.4990700.

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25

Alkahby, H. Y. "On the coronal heating mechanism by the resonant absorption of Alfven waves." International Journal of Mathematics and Mathematical Sciences 16, no. 4 (1993): 811–16. http://dx.doi.org/10.1155/s0161171293001012.

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In this paper, we will investigate the heating of the solar corona by the resonant absorption of Alfven waves in a viscous and isothermal atmosphere permeated by a horizontal magnetic field. It is shown that if the viscosity dominates the motion in a high (low)-βplasma, it creates an absorbing and reflecting layer and the heating process is acoustic (magnetoacoustic). When the magnetic field dominates the oscillatory process it creates a non-absorbing reflecting layer. Consequently, the heating process is magnetohydrodynamic. An equation for resonance is derived. It shows that resonances may occur for many values of the frequency and of the magnetic field if the wavelength is matched with the strength of the magnetic field. At the resonance frequencies, magnetic and kinetic energies will increase to very large values which may account for the heating process. When the motion is dominated by the combined effects of the viscosity and the magnetic field, the nature of the reflecting layer and the magnitude of the reflection coefficient depend on the relative strengths of the magnetic field and the viscosity.

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26

Yi, Tong, Fang Geng, and Mao Xinjie. "The X-ray Radiation Mechanism of the Compact (Neutron) Binary Stars." Symposium - International Astronomical Union 125 (1987): 249. http://dx.doi.org/10.1017/s0074180900160851.

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Usually we think a X-ray source may be a compact(neutron) binary star on which the X-ray radiation might be generated by gravitational acceleration for the particles coming from the primary and going along magnetic field lines of the compact star to the poles. But, in the past, people don't consider well the problem of particle acceleration. It seems to be simplified for the situation only to consider the gravitation effect, because some electric-magnetic effect in a strong magnetic field could not be neglected. However, it is unreasonable to neglect the plasma turbulent waves in an electric-magnetic field, because strong enough turbulent waves such as Alfven waves, whistlers generated nearby the surface of neutron stars probably contribute energy to accelerate particles, which may be more important than gravitation sometimes. For a binary system with a neutron star if ion number density N > 1017 /cm3 in its surface atmosphere, the turbulent wavess will be stimulated that will accelerate the particles reaching a speed over 108cm/s. they strike the atmosphere of the compact star in the system, so that a shock wave is formed which turns part of kinetic energy to heat to form hot spots of about 108K to emit X-ray.

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27

Malovichko, P. P. "The properties of kinetic Alfven waves and their role in the dynamics of the magnetosphere." Kosmìčna nauka ì tehnologìâ 8, no. 2s (2002): 201–6. http://dx.doi.org/10.15407/knit2002.02s.201.

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28

Shukla, Anita, and R. P. Sharma. "Nonlinear kinetic Alfven waves associated with saturating nonlinearity: applications to solar wind and coronal heating." Journal of Atmospheric and Solar-Terrestrial Physics 64, no. 5-6 (2002): 661–68. http://dx.doi.org/10.1016/s1364-6826(02)00027-5.

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29

Shi, Run, Binbin Ni, Danny Summers, Huixin Liu, Akimasa Yoshikawa, and Beichen Zhang. "Generation of Electron Acoustic Waves in the Topside Ionosphere From Coupling With Kinetic Alfven Waves: A New Electron Energization Mechanism." Geophysical Research Letters 45, no. 11 (2018): 5299–304. http://dx.doi.org/10.1029/2018gl077898.

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30

Guo, Zhifang, Minghua Hong, Yu Lin, et al. "Generation of kinetic Alfven waves in the high-latitude near-Earth magnetotail: A global hybrid simulation." Physics of Plasmas 22, no. 2 (2015): 022117. http://dx.doi.org/10.1063/1.4907666.

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31

Khalid, Saba, M. N. S. Qureshi, and W. Masood. "Compressive and rarefactive solitary structures of coupled kinetic Alfven-acoustic waves in non-Maxwellian space plasmas." Physics of Plasmas 26, no. 9 (2019): 092114. http://dx.doi.org/10.1063/1.5115478.

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32

Sadiq, Nauman, Mushtaq Ahmad, M. Farooq, and Qasim Jan. "Linear and nonlinear analysis of kinetic Alfven waves in quantum magneto-plasmas with arbitrary temperature degeneracy." Physics of Plasmas 25, no. 6 (2018): 063510. http://dx.doi.org/10.1063/1.5024829.

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33

Mithaiwala, Manish, Leonid Rudakov, Chris Crabtree, and Gurudas Ganguli. "Co-existence of whistler waves with kinetic Alfven wave turbulence for the high-beta solar wind plasma." Physics of Plasmas 19, no. 10 (2012): 102902. http://dx.doi.org/10.1063/1.4757638.

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34

Kryshtal, A. N., S. V. Gerasimenko, and A. D. Voitsekhovska. "Low-threshold instabilities of kinetic alfven waves in the chromosphere of an active region on the Sun." Kosmìčna nauka ì tehnologìâ 18, no. 5(78) (2012): 29–40. http://dx.doi.org/10.15407/knit2012.05.029.

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35

Seyler, Charles E. "Nonlinear 3-D evolution of bounded kinetic Alfven waves due to shear flow and collisionless tearing instability." Geophysical Research Letters 15, no. 8 (1988): 756–59. http://dx.doi.org/10.1029/gl015i008p00756.

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36

Wu, D. J., and L. Yang. "Nonlinear Interaction of Minor Heavy Ions with Kinetic Alfven Waves and Their Anisotropic Energization in Coronal Holes." Astrophysical Journal 659, no. 2 (2007): 1693–701. http://dx.doi.org/10.1086/512117.

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37

KALITA, LATIKA, and MANOJ KUMAR DEKA. "EFFECT OF ION TEMPERATURE ON LARGE AMPLITUDE SOLITARY KINETIC ALFVEN WAVES AND DOUBLE LAYERS IN PLASMAS WITH SUPERTHERMAL ELECTRONS." International Journal of Engineering Science and Technology 8, no. 2S (2018): 131–39. http://dx.doi.org/10.21817/ijest/2018/v10i2s/181002s024.

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38

Tsiklauri, D. "Particle acceleration by circularly and elliptically polarised dispersive Alfven waves in a transversely inhomogeneous plasma in the inertial and kinetic regimes." Physics of Plasmas 18, no. 9 (2011): 092903. http://dx.doi.org/10.1063/1.3633531.

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39

Verkhoglyadova, O., A. Agapitov, A. Andrushchenko, V. Ivchenko, S. Romanov, and Yu Yermolaev. "Compressional wave events in the dawn plasma sheet observed by Interball-1." Annales Geophysicae 17, no. 9 (1999): 1145–54. http://dx.doi.org/10.1007/s00585-999-1145-7.

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Abstract. Compressional waves with periods greater than 2 min (about 10-30 min) at low geomagnetic latitudes, namely compressional Pc5 waves, are studied. The data set obtained with magnetometer MIF-M and plasma analyzer instrument CORALL on board the Interball-1 are analyzed. Measurements performed in October 1995 and October 1996 in the dawn plasma sheet at -30 RE ≤ XGSM and |ZGSM| ≤ 10 RE are considered. Anti-phase variations of magnetic field and ion plasma pressures are analyzed by searching for morphological similarities in the two time series. It is found that longitudinal and transverse magnetic field variations with respect to the background magnetic field are of the same order of magnitude. Plasma velocities are processed for each time period of the local dissimilarity in the pressure time series. Velocity disturbances occur mainly transversely to the local field line. The data reveal the rotation of the velocity vector. Because of the field line curvature, there is no fixed position of the rotational plane in the space. These vortices are localized in the regions of anti-phase variations of the magnetic field and plasma pressures, and the vortical flows are associated with the compressional Pc5 wave process. A theoretical model is proposed to explain the main features of the nonlinear wave processes. Our main goal is to study coupling of drift Alfven wave and magnetosonic wave in a warm inhomogeneous plasma. A vortex is the partial solution of the set of the equations when the compression is neglected. A compression effect gives rise to a nonlinear soliton-like solution.Key words. Magnetosphere physics (magnetotail) · Space plasma physics (kinetic and MHD theory; non-linear phenomena)

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40

Shi, Run, and Jun Liang. "Mode conversion from kinetic Alfvén waves to modified electron acoustic waves." Physics of Plasmas 29, no. 8 (2022): 082104. http://dx.doi.org/10.1063/5.0093193.

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Possible mode conversion from kinetic Alfvén wave to modified electron acoustic wave is examined based on a multi-fluid model involving two electron populations. The mode conversion transpires when a kinetic Alfvén wave propagates through a transition between a hot-electron-dominant region and a cold-electron-dominant region. It is shown that the mode conversion and the kinetic Alfvén wave reflection depend strongly on the hot electron inertial length, the hot electron temperature, and the perpendicular wavelength. The results suggest that such conversion is ubiquitous whenever a steep gradient of electron temperature exists, for example, in the planetary auroral acceleration regions or at the boundary of the solar corona.

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41

Ghosh, G., and K. P. Das. "Three-dimensional stability of solitary kinetic Alfvé waves and ion-acoustic waves." Journal of Plasma Physics 51, no. 1 (1994): 95–111. http://dx.doi.org/10.1017/s0022377800017414.

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Starting from a set of equations that lead to a linear dispersion relation coupling kinetic Alfvén waves and ion-acoustic waves, three-dimensional KdV equations are derived for these waves. These equations are then used to investigate the three-dimensional stability of solitary kinetic Alfvén waves and ion-acoustic waves by the small-k perturbation expansion method of Rowlands and Infeld. For kinetic Alfvén waves it is found that there is instability if the direction of the plane-wave perturbation lies inside a cone, and the growth rate of the instability attains a maximum when the direction of the perturbation lies in the plane containing the external magnetic field and the direction of propagation of the solitary wave.

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42

Nagata, D., S. Machida, S. Ohtani, Y. Saito, and T. Mukai. "Solar wind control of plasma number density in the near-Earth plasma sheet: three-dimensional structure." Annales Geophysicae 26, no. 12 (2008): 4031–49. http://dx.doi.org/10.5194/angeo-26-4031-2008.

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Abstract. The plasma number density in the near-Earth plasma sheet depends on the solar wind number density and the north-south component of interplanetary magnetic field (IMF Bz) with time lag and duration of several hours. We examined the three-dimensional structure of such dependences by fitting observations of plasma sheet and solar wind to an empirical model equation. Analyses were conducted separately for northward and southward IMF conditions. Effects of solar wind speed and IMF orientation were also examined by further subdivision of the dataset. Based on obtained results, we discuss (i) the relative contribution of the ionosphere and solar wind to plasma sheet mass supply, (ii) the entry mechanisms for magnetosheath particles, and (iii) the plasma transport in the plasma sheet. We found that solar wind number density dependence is weaker and IMF Bz dependence is stronger for faster solar wind with southward IMF, which suggests the contribution of ionospheric particles. Further from the Earth, different interplanetary conditions result in different structures of solar wind dependence, which indicate different solar wind entry mechanisms: (1) southward IMF results in a strong dependence on solar wind number density in the flank high-latitude region, (2) slow solar wind with northward IMF leads to lower-latitude peaks of solar wind number density dependence in the flank region, (3) fast solar wind with northward IMF results in a strong dependence on solar wind number density at the down-tail dusk flank equator, and (4) solar wind number density dependence is stronger in the downstream of quasi-parallel bow shock. These features are attributable to (1) low-latitude dayside reconnection entry, (2) high-latitude dayside reconnection entry, (3) entry due to decay of Kelvin-Helmholtz vortices, and (4) diffusive entry mediated by kinetic Alfven waves, respectively. Effect of IMF Bz and its time lags show plasma sheet reconfiguration associated with enhanced convective transport under southward IMF. Duration of IMF Bz effect under northward IMF is interpreted in terms of turbulent diffusive transport.

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43

Jatenco-Pereira, V., A. C. L. Chian, and N. Rubab. "Alfvén waves in space and astrophysical dusty plasmas." Nonlinear Processes in Geophysics 21, no. 2 (2014): 405–16. http://dx.doi.org/10.5194/npg-21-405-2014.

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Abstract. In this paper, we present some results of previous works on Alfvén waves in a dusty plasma in different astrophysical and space regions by taking into account the effect of superthermal particles on the dispersive characteristics. We show that the presence of dust and superthermal particles sensibly modify the dispersion of Alfvén waves. The competition between different damping processes of kinetic Alfvén waves and Alfvén cyclotron waves is analyzed. The nonlinear evolution of Alfvén waves to chaos is reviewed. Finally, we discuss some applications of Alfvén waves in the auroral region of space plasmas, as well as stellar winds and star-forming regions of astrophysical plasmas.

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44

SHUKLA, P. K., NITIN SHUKLA, and L. STENFLO. "Kinetic modulational instability of broadband dispersive Alfvén waves in plasmas." Journal of Plasma Physics 73, no. 2 (2007): 153–57. http://dx.doi.org/10.1017/s0022377806006271.

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Abstract.We consider a kinetic modulational instability of broadband (random phase) magnetic-field-aligned circularly polarized dispersive Alfvén waves in plasmas. By treating random phase Alfvén waves as quasi-particles, we consider their nonlinear interactions with ion quasi-modes within the framework of the wave-kinetic and Vlasov descriptions. A nonlinear dispersion relation governing such interactions is derived and analyzed. An explicit expression for the kinetic modulational instability growth rate is presented. Our results can be of relevance to the nonlinear propagation of incoherent Alfvén waves, which have been frequently observed in interstellar media, in the solar corona and in the solar wind, as well as in the foreshock regions of planetary bow-shocks and laboratory plasmas.

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45

Roberts, Owen W., Yasuhito Narita, and C. Philippe Escoubet. "Multi-scale analysis of compressible fluctuations in the solar wind." Annales Geophysicae 36, no. 1 (2018): 47–52. http://dx.doi.org/10.5194/angeo-36-47-2018.

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Abstract. Compressible plasma turbulence is investigated in the fast solar wind at proton kinetic scales by the combined use of electron density and magnetic field measurements. Both the scale-dependent cross-correlation (CC) and the reduced magnetic helicity (σm) are used in tandem to determine the properties of the compressible fluctuations at proton kinetic scales. At inertial scales the turbulence is hypothesised to contain a mixture of Alfvénic and slow waves, characterised by weak magnetic helicity and anti-correlation between magnetic field strength B and electron density ne. At proton kinetic scales the observations suggest that the fluctuations have stronger positive magnetic helicities as well as strong anti-correlations within the frequency range studied. These results are interpreted as being characteristic of either counter-propagating kinetic Alfvén wave packets or a mixture of anti-sunward kinetic Alfvén waves along with a component of kinetic slow waves. Keywords. Interplanetary physics (MHD waves and turbulence)

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46

Yinhua, Chen, Lu Wei, and M. Y. Yu. "Nonlinear dust kinetic Alfvén waves." Physical Review E 61, no. 1 (2000): 809–12. http://dx.doi.org/10.1103/physreve.61.809.

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47

Nariyuki, Y., T. Umeda, T. K. Suzuki, and T. Hada. "Ion acceleration by parallel propagating nonlinear Alfvén wave packets in a radially expanding plasma." Nonlinear Processes in Geophysics 21, no. 1 (2014): 339–46. http://dx.doi.org/10.5194/npg-21-339-2014.

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Abstract. The numerical simulation of the nonlinear evolution of the parallel propagating Alfvén waves in a radially expanding plasma is performed by using a kinetic-fluid model (the Vlasov–MHD model). In our study, both the nonlinear evolution of the Alfvén waves and the radial evolution of the velocity distribution function (VDF) are treated simultaneously. On the other hand, important ion kinetic effects such as ion cyclotron damping and instabilities driven by the non-equilibrium ion velocity distributions are not included in the present model. The results indicate that the steepened Alfvén wave packets outwardly accelerate ions, which can be observed as the beam components in the interplanetary space. The energy of imposed Alfvén waves is converted into the longitudinal fluctuations by the nonlinear steepening and the nonlinear Landau damping. The wave shoaling due to the inhomogeneity of the phase velocity is also observed.

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48

KALITA, B. C., and R. P. BHATTA. "Kinetic Alfvén solitons in a low-beta plasma." Journal of Plasma Physics 57, no. 2 (1997): 235–45. http://dx.doi.org/10.1017/s0022377896004849.

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Kinetic Alfvén solitons with hot electrons and finite electron inertia in a low-beta (β=8πn0T/B2G, the ratio of the kinetic to the magnetic pressure) plasma is studied analytically, with the ion motion being considered dominant through the polarization drift. Both compressive and rarefactive kinetic Alfvén solitons are found to exist within a definite range of kz (the direction of propagation of the kinetic Alfvén solitary waves with respect to the direction of the magnetic field) for each pair of assigned values of β and M (Mach number). Unlike in previous theoretical investigations, β appears as an explicit parameter for the kinetic Alfvén solitons in this case. In addition, consideration of the electron pressure gradient is found to suppress the speed of both the Alfvén solitons considerably for A (=2QM2/βk2z, with Q the electron-to-ion mass ratio) less than unity.

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49

BINGHAM, R., P. K. SHUKLA, B. ELIASSON, and L. STENFLO. "Solar coronal heating by plasma waves." Journal of Plasma Physics 76, no. 2 (2009): 135–58. http://dx.doi.org/10.1017/s0022377809990031.

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AbstractThe solar coronal plasma is maintained at temperatures of millions of degrees, much hotter than the photosphere, which is at a temperature of just 6000 K. In this paper, the plasma particle heating based on the kinetic theory of wave–particle interactions involving kinetic Alfvén waves and lower-hybrid drift modes is presented. The solar coronal plasma is collisionless and therefore the heating must rely on turbulent wave heating models, such as lower-hybrid drift models at reconnection sites or the kinetic Alfvén waves. These turbulent wave modes are created by a variety of instabilities driven from below. The transition region at altitudes of about 2000 km is an important boundary chromosphere, since it separates the collision-dominated photosphere/chromosphere and the collisionless corona. The collisionless plasma of the corona is ideal for supporting kinetic wave–plasma interactions. Wave–particle interactions lead to anisotropic non-Maxwellian plasma distribution functions, which may be investigated by using spectral analysis procedures being developed at the present time.

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Marsch, Eckart. "Solar wind and kinetic heliophysics." Annales Geophysicae 36, no. 6 (2018): 1607–30. http://dx.doi.org/10.5194/angeo-36-1607-2018.

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Abstract. This paper reviews recent aspects of solar wind physics and elucidates the role Alfvén waves play in solar wind acceleration and turbulence, which prevail in the low corona and inner heliosphere. Our understanding of the solar wind has made considerable progress based on remote sensing, in situ measurements, kinetic simulation and fluid modeling. Further insights are expected from such missions as the Parker Solar Probe and Solar Orbiter. The sources of the solar wind have been identified in the chromospheric network, transition region and corona of the Sun. Alfvén waves excited by reconnection in the network contribute to the driving of turbulence and plasma flows in funnels and coronal holes. The dynamic solar magnetic field causes solar wind variations over the solar cycle. Fast and slow solar wind streams, as well as transient coronal mass ejections, are generated by the Sun's magnetic activity. Magnetohydrodynamic turbulence originates at the Sun and evolves into interplanetary space. The major Alfvén waves and minor magnetosonic waves, with an admixture of pressure-balanced structures at various scales, constitute heliophysical turbulence. Its spectra evolve radially and develop anisotropies. Numerical simulations of turbulence spectra have reproduced key observational features. Collisionless dissipation of fluctuations remains a subject of intense research. Detailed measurements of particle velocity distributions have revealed non-Maxwellian electrons, strongly anisotropic protons and heavy ion beams. Besides macroscopic forces in the heliosphere, local wave–particle interactions shape the distribution functions. They can be described by the Boltzmann–Vlasov equation including collisions and waves. Kinetic simulations permit us to better understand the combined evolution of particles and waves in the heliosphere.

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