Spectral characteristics of plasma sheet ion and electron populations during undisturbed geomagnetic conditions

Abstract

We analyze 127 one‐hour average samples of central plasma sheet ions and electrons in order to determine spectral characteristics of these magnetotail particle populations during periods of low geomagnetic activity (AE<100 nT). Particle data from the low energy proton and electron differential energy analyzer (LEPEDEA) and medium energy particle instrument (MEPI) on ISEE 1 were combined to obtain differential energy spectra in the plasma sheet at geocentric radial distances R>12 RE. We find that, for even the longest periods sampled, the nearly isotropic central plasma sheet total ion and electron populations were measured to be continuous particle distributions from our lowest energy of tens of eV/e to a few hundred keV. The kappa distribution function (f ∼ [1 + E/κEo]−κ−1, where Eo, the energy of the peak differential number flux (measured in particles/cm² s sr keV), is related to the temperature through κ, a constant) most often reproduces the observed differential energy spectra. Spectra dominated by a single kappa functional form are observed during 83 (99) hours for ions (electrons). Spectra which are not dominated by a single kappa functional form can usually be closely approximated by superposed kappa functional forms. For both ions and electrons κ is typically in the range 4–8, with a most probable value between 5 and 6, so that the spectral shape is distinctly non‐Maxwellian. Eoi and Eoe are highly correlated, whereas κi and κe are not correlated; κi is roughly proportional to Eoi½, whereas κe is not correlated with Eoe. We statistically investigate the importance of flux and energy contributions from extramagnetospheric sources by separately analyzing intervals when simultaneously measured interplanetary particle fluxes are either enhanced or at low levels. A linear superposition of plasma sheet fluxes and interplanetary fluxes that have entered the magnetosphere is observed. The presence of interplanetary particles does not affect the average values of plasma sheet Eo or κ. We conclude that for AE<100 nT the nonthermal shape of plasma sheet particle distributions results from ongoing magnetospheric processes which are probably independent of geomagnetic activity as measured by AE.

Shaping the solar wind temperature anisotropy by the interplay of electron and proton instabilities

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A one dimensional, electrostatic Vlasov model for the generation of suprathermal electron tails in solar wind conditions

“…In particular, their charged particle velocity distributions usually differ from simple Maxwellian distributions and exhibit a great variety of anisotropies and components such as suprathermal beams and tails [see Christon et al, 1989;Collier, 1999;Maksimovic et al, 2005] which have been a rich source of problems for space physics research.…”

Proton and heavy ion acceleration by stochastic fluctuations in the Earth's magnetotail

“…Energies from tens of keV to a few hundreds of keV are found in the Earth's magnetotail (Christon et al, 1989;Keiling et al, 2004;Imada et al, 2007;Haaland et al, 2010;Artemyev et al, 2014). Heavy ions like singly charged oxygen O + are also observed in the magnetotail, with energies often reaching several hundred keV (Keika et al, 2013;Kronberg et al, 2014Kronberg et al, , 2015.…”

“…Heavy ions like singly charged oxygen O + are also observed in the magnetotail, with energies often reaching several hundred keV (Keika et al, 2013;Kronberg et al, 2014Kronberg et al, , 2015. Further, relevant levels of energetic electrons and ions are also observed during periods of low geomagnetic activity (Christon et al, 1989), leaving open the search for the acceleration mechanism. In addition, the observed proton temperatures, of the order of 5-10 keV, are also much larger than the energy corresponding to their original source, but the mechanism that can generate such heated particles is not fully understood (Runov et al, 2006;Artemyev et al, 2011).…”