https://ogma.newcastle.edu.au/vital/access/ /manager/Index ${session.getAttribute("locale")} 5 https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:53322 Wed 22 Nov 2023 10:05:08 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:20212 Wed 11 Apr 2018 16:40:32 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:3308 Wed 11 Apr 2018 16:15:14 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:2001 Wed 11 Apr 2018 14:39:39 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:10963 Wed 11 Apr 2018 13:47:58 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:13514 v^g, with the radial electric field component in the equatorial plane of the magnetosphere, e_v^eq, via the fields in the ionosphere. In this paper we use a fully coupled ULF wave model to determine the ratio e_v^eq/b_v^g for a 5 mHz FLR formed at high latitudes. We find that Ozeke et al. (2009) underestimated the ULF wave magnetic field on the ground which varies with ionosphere Hall conductance. This difference is found to be caused by assuming a decoupled wave mode model for the ionosphere fields. Any relationship that involves ULF wavefields in the ionosphere must include the effects of ULF wave mode mixing.]]> Wed 11 Apr 2018 12:31:29 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:4837 Wed 11 Apr 2018 12:12:48 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:13515 y indices of 50, 100, 250, and 600 corresponding to the risk levels of “low,” “moderate,” “high,” and “extreme,” respectively. Analysis of GIC_y indices derived from Australian magnetometer data shows that only southern Australian regions reached the “moderate” risk levels defined in this study with mainland southern Australia stations reaching this risk level twice over the previous two solar cycles. Southern Australian regions such as Tasmania reached moderate levels approximately 20 times during the previous solar cycle. Furthermore, elevated risk levels are typically only observed in Australia during solar maximum and its decline phase.]]> Wed 11 Apr 2018 11:49:40 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:27694 10 keV electrons during the early recovery phase of a moderate geomagnetic storm. We find that internal energization of equatorially mirroring electrons via nonresonant ULF wave-particle interactions can explain these observations. The wave poloidal components cause radial drift of electrons, increasing (decreasing) their kinetic energy as they move inward (outward). Electrons with initial kinetic energies of a few keV can be energized to double these values within an hour by interaction with the 3 mHz waves. The energization rate is somewhat less for the 4-5 mHz waves. An increase in the ionospheric conductance decreases the power of the fast mode wave, reducing radial drift velocities and hence decreasing the rate of energization. The fast mode poloidal field varies with radial distance and longitude, and this also affects energization. Electrons which drift outward encounter a region where the toroidal field due to the field line resonance becomes dominant and produces strong azimuthal drift. These electrons become trapped in an L-shell range just outward of the resonance region and are not energized.]]> Wed 11 Apr 2018 11:43:08 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:884 Wed 11 Apr 2018 11:22:14 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:14007 Wed 11 Apr 2018 10:54:18 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:1122 Wed 11 Apr 2018 10:02:11 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:1128 Wed 11 Apr 2018 09:58:59 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:1526 Wed 11 Apr 2018 09:34:00 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:43961 Wed 05 Oct 2022 14:01:22 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:37696 Tue 16 Mar 2021 17:37:59 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:11564 Sat 24 Mar 2018 08:14:01 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:29480 E region can reduce the chance of F region and increase the chance of E region backscatter. It was also shown that reduction in backscatter cannot be explained by D region absorption. Using a normalized SYM-H value, percentage time through recovery phase can be estimated during storm progression which allows a prediction of backscatter return in real time that accounts for varying storm recovery phase duration.]]> Sat 24 Mar 2018 07:29:45 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:26414 Sat 24 Mar 2018 07:27:57 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:27559 Sat 24 Mar 2018 07:23:30 AEDT ]]>