Isotropic boundary, IB - last update: 4 September 1996, 1015 UT (RR)


IB Observations of precipitating (Jp) and trapped (Jt) energetic (> 30 keV) particle fluxes at the ionospheric altitudes within the auroral oval region has revealed the existence of a sharp boundary separating the poleward zone of isotropic precipitation (Jp = Jt) from the equatorward zone of weak loss cone filling (Jp << Jt) at all local times (Sergeev and Malkov, 1988). By definition, this boundary is called the isotropic boundary, IB. They have been studied mainly using the NOAA satellites in polar orbit at the altitude of about 800 km.

Sometimes, especially after substorms, a region of rather intense proton precipitation is observed equatorward of IB (Gvozdevsky et al., 1997). These regions have been called low-latitude proton precipitation (LLPP) regions.


Basic characteristics of isotropic boundaries are (Sergeev et al., 1993):


High precipitation fluxes at the top of the ionosphere indicate efficient scattering of particles into the narrow loss cone in the magnetosphere. Although fluctuating electric and magnetic fields could produce the needed pitch angle scattering, the more probable mechanisms for isotropic boundaries is the tail current sheet scattering (TCS). It is based on the fact that magnetic field lines at higher latitudes have increasingly non-dipolar shape which, together with non-zero particle gyroradius, leads to non-adiabatic (stochastic) particle motion at the equator in the central plasma sheet. The isotropic boundary is thus the boundary between the inner magnetospheric region of adiabatic particle motion, and the outer region of stochastic particle motion in the equatorial tail current sheet. The IB characteristics listed above agree with this interpretation.

The threshold condition for strong pitch angle scattering to the center of loss cone is R/r < 8, where R is the curvature radius of the field line, and r the effective particle gyroradius, G/Bz. It can be shown that R/r depends strongly on particle rigidigy G and equatorial Bz.


The dependance of IB position of equatorial Bz makes it a potential remote sensing tool for equatorial magnetic field from low altitudes. In addition, the isotropic boundary analysis can be used to map the auroral oval down to the magnetosphere by comparing the IB positions with lower energy auroral precipitation regions. The IB of >30 keV protons is found in the diffuse region (equatorward half of the oval) on the nightside, and equatorward of the intense auroral precipitation at dayside and dusk. On the other hand, the IB of >30 keV electrons on the nightside is often found in the structured precipitation region (poleward half), or just equatorward from it. (Yahnin et al., ICS-3). This implies that the diffuse aurora map to the dipole-like region close to Earth, while discrete auroras map to the current sheet region (Bz < 5 nT). Arcs are often found in wide latitudinal range, most likely covering both near-Earth plasma sheet and PSBL. Common feature in all cases is the small Bz value indicating current sheet precense.


See also: