https://nova.newcastle.edu.au/vital/access/ /manager/Index en-au 5 https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:40513 Wed 13 Jul 2022 15:09:51 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:16955 Wed 11 Apr 2018 16:56:09 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:392 Wed 11 Apr 2018 15:05:58 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4432 65 degrees during northward IMF; there is marked contrast between currents for northward and southward IMF but the evolution of the patterns is continuous with IMF rotation. The directions of flows inferred from the most poleward currents are more consistent with theoretical expectations of transport away from magnetopause reconnection than previous results. We attribute the differences to the restriction in this analysis to intervals having relatively stable distributions of current so that the data set corresponds more nearly to pure states of the system.]]> Wed 11 Apr 2018 15:05:45 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:7916 0.]]> Wed 11 Apr 2018 13:26:57 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3306 Wed 11 Apr 2018 13:13:10 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3307 Wed 11 Apr 2018 13:12:07 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3499 Wed 11 Apr 2018 12:31:12 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:11505 y/B_z)) 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, E_yz; 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 E_yz 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 E_yz. 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 ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3312 Wed 11 Apr 2018 10:28:10 AEST ]]> 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 ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:1127 Sat 24 Mar 2018 08:32:03 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:39701 Fri 17 Jun 2022 16:42:03 AEST ]]>