The role of higher-order modes on the electromagnetic whistler-cyclotron wave fluctuations of thermal and non-thermal plasmas

Kinetic transverse dispersion relation for relativistic magnetized electron-positron plasmas with Maxwell-Jüttner velocity distribution functions

“…Furthermore, in the simulation results, we can see the spontaneous thermal fluctuations, which have been described in previous works for unmagnetized relativistic plasmas [22][23][24] and for magnetized nonrelativistic plasmas, in proton 28 and electron 29 scales. In the nonrelativistic limit, it has been shown that spontaneous fluctuations are enhanced and shifted to smaller wave numbers for higher plasma beta values, 28,29 which is consistent with our simulations. Because the relationship between the plasma beta b ¼ 8pnk B T=B 2 0 and l is given by l ¼ ð2=bÞðx 2 pe =X 2 c Þ, and for x pe /X c ¼ 1, we obtain l ¼ 2/b, which means that our examples correspond to b ¼ 0.02 and 0.2, respectively.…”

Theory of electromagnetic fluctuations for magnetized multi-species plasmas

“…This feature agrees with previous results. [18][19][20] Because of the condition K À ¼ 0 [see Eqs. (32)-(35)], the electromagnetic fluctuation level exhibits intense peaks near the modes with ImðxÞ $ 0.…”

“…4,[18][19][20] The parallel propagating thermally induced magnetic fluctuations seem to be a relevant contribution to the solar wind plasma under conditions stable to anisotropydriven instabilities. 20 However, we expect that fluctuations with k ?…”

“…Araneda et al 18 and Viñas et al 19 studied magnetic fluctuations associated to Alfv en and whistler waves, respectively, in isotropic Maxwellian plasmas, and showed that heavily damped modes of the dispersion relation may play an important role in the emission and absorption of plasma fluctuations since they seem to constrain the structure of the fluctuation spectra. Navarro et al 20 extended these ideas to anisotropic but quasi-stable bi-Maxwellian plasmas, showing that these fluctuations may be related to the fluctuating magnetic power observed in the solar wind below the linear instability thresholds.…”

Amplification of Collective Magnetic Fluctuations in Magnetized Bi-Maxwellian Plasmas for Parallel Wave Vectors. I. Electron–proton Plasma

“…However, it can be substantially simplified assuming that the wave vector is directed along the ambient magnetic field . Making use of this assumption, several authors recently analyzed the magnetic fluctuation spectrum for parallel wave vectors in a plasma with a bi-Maxwellian or bi-Kappa velocity distribution function (Navarro et al 2014a(Navarro et al , 2014bViñas et al 2014Viñas et al , 2015Kim et al 2016). Yet, those results are valid only for non-collective plasma modes (noneigenmodes).…”