https://nova.newcastle.edu.au/vital/access/ /manager/Index en-au 5 Science data products for AMPERE https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:40513 Wed 13 Jul 2022 15:09:51 AEST ]]> Development of large-scale Birkeland currents determined from the active magnetosphere and planetary electrodynamics response experiment https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:16955 Wed 11 Apr 2018 16:56:09 AEST ]]> High-latitude electromagnetic and particle energy flux during an event with sustained strongly northward IMF https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:392 Wed 11 Apr 2018 15:05:58 AEST ]]> Seasonal and interplanetary magnetic field dependence of the field-aligned currents for both Northern and Southern Hemispheres https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:7916 0.]]> Wed 11 Apr 2018 13:26:57 AEST ]]> Comparison of large-scale Birkeland currents determined from Iridium and SuperDARN data https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3306 Wed 11 Apr 2018 13:13:10 AEST ]]> Technique: large-scale ionospheric conductance estimated from combined satellite and ground-based electromagnetic data https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3499 Wed 11 Apr 2018 12:31:12 AEST ]]> Statistical analysis of the dependence of large-scale Birkeland currents on solar wind parameters https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:11505 y/Bz)) since this governs the spatial morphology of the currents. The Birkeland current densities were then corrected for variations in EUV-produced ionospheric conductance by normalizing the current densities to those occurring for 0° dipole tilt. To determine the dependence of the currents on other solar wind variables for a given IMF clock angle, the data were then sorted sequentially by the following parameters: the solar wind electric field in the plane normal to the Earth–Sun line, Eyz; the solar wind ram pressure; and the solar wind Alfvén Mach number. The solar wind electric field is the dominant factor determining the Birkeland current intensities. The currents shift toward noon and expand equatorward with increasing solar wind electric field. The total current increases by 0.8 MA per mV m⁻¹ increase in Eyz for southward IMF, while for northward IMF it is nearly independent of the electric field, increasing by only 0.1 MA per mV m⁻¹ increase in Eyz. The dependence on solar wind pressure is comparatively modest. After correcting for the solar dynamo dependencies in intensity and distribution, the total current intensity increases with solar wind dynamic pressure by 0.4 MA/nPa for southward IMF. Normalizing the Birkeland current densities to both the median solar wind electric field and dynamic pressure effects, we find no significant dependence of the Birkeland currents on solar wind Alfvén Mach number.]]> Wed 11 Apr 2018 11:29:24 AEST ]]> Global observations of electromagnetic and particle energy flux for an event during northern winter with southward interplanetary magnetic field https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4433 Wed 11 Apr 2018 10:29:48 AEST ]]> A comparison of small-scale magnetic fluctuations in the Region 1 and 2 field-aligned current systems https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:33035 y, indicating a connection between the R1 fluctuation and the driving solar wind most likely explained by magnetic reconnection; and (4) high‐frequency fluctuations in R2 are enhanced in a small region near local noon and respond clearly to nightside drivers, as characterized by the auroral electrojet index. Our analysis shows that the intensity of R1 and R2 high‐frequency magnetic fluctuations is directly connected to the intensity of FACs, which implies that the magnetic fluctuations are closely related to the magnetospheric processes that drive them.]]> Tue 03 Sep 2019 18:23:38 AEST ]]>