Determination of auroral electrostatic potentials using high‐ and low‐altitude particle distributions

Abstract

The Dynamics Explorer (DE) pair of spacecraft provide a unique opportunity to search for the presence of electric fields aligned parallel to magnetic field lines by sampling, nearly simultaneously, the velocity‐space distribution functions of ions and electrons at two points on auroral field lines: DE 1 at high altitudes (9000–15,000 km in this study) and DE 2 at low altitudes (400–800 km). Three independent techniques are used to infer the auroral electrostatic potential difference from the particle distributions: (1) the energy of the precipitating electrons at DE 2 (compared to that at DE 1), (2) the energy of the upgoing ions at DE 1, and (3) the widening of the loss cone for electrons at DE 1. The three estimates are in general agreement, confirming the long‐standing, but not fully accepted, hypothesis that parallel electrostatic fields of 1–10 kV potential drop at 1–2 RE altitude are an important source for auroral particle acceleration. The upflowing ion distribution typically can be characterized by a sharp peak and a falloff at high energies of the form exp‐{(E‐Epeak)/Eo}, with Epeak being the peak energy and Eo the characteristic energy. This is the functional dependence one expects if a Maxwellian of thermal energy Eo is accelerated upward by a parallel electric field with eΦ=Epeak. The fact that the peak energies and not the flow velocities of the various ion species are in agreement also lends strong credence to the parallel electric field hypothesis. The acceleration mechanism cannot be a simple parallel electric field, however, for two reasons: first, the characteristic energy Eo is considerably larger than the ionospheric thermal energy (Eo is typically hundreds of electron volts and 20–30% of Epeak), and second, the energy Epeak is typically 30–50% smaller than that inferred by the two other independent techniques. The distribution does appear to be consistent with an ionospheric source, heated within (or above) the acceleration region, since the ion average energy is comparable to eΦ. The average energies of O+ and He+ are comparable to, but typically somewhat larger than, that of H+, indicating that a two‐stream instability may be the heating mechanism. Electron heating is also detected within the auroral acceleration region, with gains in characteristic energies of 10–15% of eΦ. From the high‐altitude electron measurements, we can determine a minimum potential distribution as a function of altitude in order to overcome the mirror force. We find that in one case at least 9M V of the 2300‐V potential drop must occur above 7000 km, and at least 960 V above 2000 km.

Particle simulation of the auroral zone showing parallel electric fields, waves, and plasma acceleration

“…This can be seen in [Reiff et al, 1986[Reiff et al, , 1988[Reiff et al, , 1993. Our simulation results show that inflowing ion beams from the magnetotail can generate potential drops of up to 2.7 kV over an altitude range of a few thousand kilometers (see Figure 5).…”

“…Observations have indicated, however, that microscale wave-particle interactions play an active role in dissipating and transferring energy in the auroral zone from beam kinetic energy to thermal energy via plasma waves [Reiff et al, 1986[Reiff et al, , 1988 The study here examines both the formation of semiglobal quasi-static parallel electric fields and microscale wave particle interactions in a self-consistent particle-in-cell simulation. This approach differs from static equilibria models constructed for adiabatic conditions [Chiu and Cornwall, 1980;Lyons, 1981;Newman et al, 1986;Cornwall, 1990], kinetic Alfv6n wave models [Lysak and Dum, 1983;Lysak, 1985Lysak, , 1993Kletzing, 1994] [Yamamoto and Kan, 1985], and the investigation of anisotropic magnetotail distributions as a driver for auroral processes [Winglee et al, 1988].…”

parallel electric fields in discrete arcs

“…Subsequent missions verified this finding. The results from the Dynamics Explorer (DE) mission suggested that there were possibly two acceleration layers [Reiff et al, 1988 and references therein; Gurgiolo and Burch, 1988]. FAST observations also suggest both highand low-altitude acceleration regions ].…”

Outflow of low-energy O<sup>+</sup> ion beams observed during periods without substorms

“…The results indicate that ions are not only accelerated by the potential, but they are also heated. Mass-dependent heating has been observed previously (Collin, 1987;Reiff et al, 1988;Möbius et al, 1998;Cui et al, 2010), but the details of how such a heating mechanism works still remains unknown. Note that for the O + we observed, there are counts in channels in the adjacent bins relative to the magnetic field direction and the temperature calculation includes their contribution.…”