The Sudbury Neutrino Observatory (SNO) used an array of 3 He proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (ν x ) 8 B solar neutrino flux. This technique is independent of previous methods employed by SNO The Sudbury Neutrino Observatory [1] detects 8 B solar neutrinos through three reactions: charged-current interactions (CC) on deuterons, in which only electron neutrinos participate; neutrino-electron elastic scattering (ES), which are dominated by contributions from electron neutrinos; and neutral-current (NC) disintegration of the deuteron by neutri-

[1] The ionosphere provides a large and variable fraction of the plasma that makes up the Earth's magnetosphere. The sparseness of ion outflow observations and limitations of global magnetospheric models have limited progress in understanding how spatial and temporal variations in the ionospheric component of the magnetosphere affects magnetospheric processes such as storms and substorms. Moreover, because existing comprehensive ion outflow data sets are not organized in terms of large-scale, dynamic, magnetospheric features, they cannot be used as boundary conditions or ground truth for large-scale magnetospheric models. This paper presents a method to self-consistently generate dynamic auroral zone boundaries from ion and electron data obtained on the same platform with mass-resolved ion outflow observations. We show that this dynamic coordinate system can be used to organize the ion outflow observations so that they are compatible to use with large-scale magnetospheric models.

[1] We have surveyed one year of northern hemisphere data from the FAST satellite and obtained the first global estimates of the characteristic energy of the energetic oxygen ion outflows and their relative distribution within the auroral oval. Recent results have shown that, above $3,000 km, the FAST/TEAMS instrument covers the energy range that includes almost all of the escaping O + . The highest mean characteristic O + energy is found at the poleward edge of the night-side auroral oval. Our results suggest that the energization and/or transport are operating differently in the noon, dusk, midnight and dawn sectors of the auroral oval. The results presented here also provide required ground truth and boundary conditions for global modeling. Citation: Andersson, L., W. K. Peterson, and K. M.McBryde (2005), Estimates of the suprathermal O + outflow characteristic energy and relative location in the auroral oval, Geophys. Res. Lett., 32, L09104,