https://nova.newcastle.edu.au/vital/access/ /manager/Index ${session.getAttribute("locale")} 5 https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3254 Wed 11 Apr 2018 17:06:56 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:6845 Wed 11 Apr 2018 17:04:44 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3308 Wed 11 Apr 2018 16:15:14 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:17076 30 keV electron precipitation flux of 5.6 × 10⁷ el. cm⁻² sr⁻¹ s⁻¹ and a spectral gradient consistent with that observed by THEMIS, it was possible to accurately reproduce the peak observed riometer absorption at Macquarie Island (L = 5.4) and the associated NWC radio wave phase change observed at Casey, Antarctica, during the second, larger substorm. The flux levels were near to 80% of the peak fluxes observed in a similar substorm as studied by Clilverd et al. (2008). During the initial stages of the second substorm, a latitude region of 5 < L < 9 was affected by electron precipitation. Both substorms showed expansion of the precipitation region to 4 < L < 12 more than 30 min after the injection. While both substorms occurred at similar local times, with electron precipitation injections into approximately the same geographical region, the second expanded in an eastward longitude more slowly, suggesting the involvement of lower-energy electron precipitation. Each substorm region expanded westward at a rate slower than that exhibited eastward. This study shows that it is possible to successfully combine these multi-instrument observations to investigate the characteristics of substorms.]]> Wed 11 Apr 2018 16:05:29 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3400 Wed 11 Apr 2018 15:32:00 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:15977 Wed 11 Apr 2018 13:53:31 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:17160 Wed 11 Apr 2018 13:48:48 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3258 Wed 11 Apr 2018 13:39:04 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:1874 Wed 11 Apr 2018 13:08:15 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:1137 Wed 11 Apr 2018 13:05:54 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:14371 137Cs) technique has been used successfully in many parts of the world to estimate net (ca. 30–50 years) soil redistribution by wind and water erosion and tillage activities. The point‐based technique has hitherto been confined largely to individual fields and hillslopes, particularly in Australia. Its application here to the Australian continent (≈5 km grid) was achieved using geostatistics and nationally coordinated measurements (early 1990s) from ≈200 locations at the ≈1 km scale. A map of the ¹³⁷Cs reference inventory for Australia has been previously established. Sequential indicator co‐simulation of the ¹³⁷Cs inventory and the Australian Soil Classification was used to estimate net (between mid‐1950s and early 1990s) soil redistribution using the Australian Empirical Model. This geostatistical approach showed that nearly five times more soil was lost from cultivated land (−4.29 to +0.17t ha^-1 yr^-1) than from uncultivated (−0.91 to +0.05t ha^-1yr^-1) land in Australia. This information on spatial uncertainty is essential for regional soil management to assess the risk to soil conservation. Soil erosion exceeding a tolerable threshold value (e.g., 0.5 t ha^-1 yr^-1) occurred over 16% of Australia, mainly in cultivated regions (median = −1.26t ha^-1yr^-1). Soil erosion estimates are neglected in carbon balances for greenhouse gas abatement and carbon accounting models. Reliable quantitative data on the recent extent and rates of soil erosion are needed to underpin the selection of effective soil conservation measures, to inform carbon balances and to understand regional soil function for sustainable agricultural systems.]]> Wed 11 Apr 2018 13:01:35 AEST ]]> https://nova.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://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:7306 Wed 11 Apr 2018 12:25:38 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4837 Wed 11 Apr 2018 12:12:48 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10964 2 MeV electron flux observed at geosynchronous orbit, starting at 00 UT on 25 June 2008, is attributed to a rapid (1–4 h) nonadiabatic loss process. ULF waves were observed by the THEMIS-A, -D, and -E probes in the afternoon-to-dusk sector from the magnetopause to geosynchronous altitude. Estimates of the electron resonant energies indicate strong drift resonant interactions occurring between the energetic electrons and the observed waves. The rate of outward radial diffusion was estimated for MeV electrons using the observed ULF wave azimuthal electric field and compressional magnetic field and the diffusion time (~2.5 h) was found to be in good agreement with the observed time for nonadiabatic flux decreases at geosynchronous orbit. The magnetopause was compressed inside of its nominal position because of increased solar wind dynamic pressure. The electron loss is interpreted as a combination of magnetopause shadowing (from the compressed magnetosphere) and enhanced outward diffusion from ULF wave-particle drift resonant interactions. The enhanced day-night asymmetry of the MeV electron drift path from the compression suggests that enhanced losses may have also occurred around local noon as well as in the afternoon-to-dusk sector.]]> Wed 11 Apr 2018 11:48:02 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4836 Wed 11 Apr 2018 11:44:59 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:17159 Wed 11 Apr 2018 11:41:53 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4831 Wed 11 Apr 2018 10:57:25 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:2003 Wed 11 Apr 2018 10:37:04 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:6847 Wed 11 Apr 2018 10:21:51 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:7281 Wed 11 Apr 2018 10:18:13 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4834 Wed 11 Apr 2018 10:16:13 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:1122 Wed 11 Apr 2018 10:02:11 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:1128 Wed 11 Apr 2018 09:58:59 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:17071 Wed 11 Apr 2018 09:19:38 AEST ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:7819 Sat 24 Mar 2018 08:37:35 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:7818 Sat 24 Mar 2018 08:37:35 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:867 Sat 24 Mar 2018 08:31:31 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3023 Sat 24 Mar 2018 08:30:02 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:1986 Sat 24 Mar 2018 08:27:08 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:2444 Sat 24 Mar 2018 08:26:53 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10740 3.3. Plasmaspheric refilling progressed with a clear diurnal variation associated with linearly increasing plasma density in the daytime and decreasing plasma density at nighttime. The daytime increases in plasma mass density related to refilling rates ranging from ~250 to ~13 amu cm⁻³ h⁻¹ over L = 2.3–3.8. The resultant upward plasma flux at the 1000 km level was in the range 0.9–5.2 × 10⁸ amu cm⁻² s⁻¹. We also determined the daily averaged refilling rate to be ~420 amu cm⁻³ d⁻¹ at L = 2.9–3.1, including the nighttime downward flux. By comparison with Imager for Magnetopause-to-Aurora Global Exploration–EUV and VLF whistler data we were able to estimate the plasma composition and found the O⁺ proportion was of order 3%–7% at L = 2.3 and 6%–13% at L = 3.0.]]> Sat 24 Mar 2018 08:14:29 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10682 Sat 24 Mar 2018 08:09:30 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10987 Sat 24 Mar 2018 08:07:56 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10989 300 keV and ~1 MeV trapped electrons, and also consistent with the daily average ULF (ultralow frequency) Pc1–2 power (L = 3.9) from Lucky Lake, Canada, which was elevated during the ~1 MeV electron precipitation period. This suggests that Pc1–2 waves may play a role in outer radiation belt loss processes during this interval. We show that the >300 keV trapped electron flux from POES is a reasonable proxy for electron precipitation during recurrent high-speed solar wind streams, although it did not describe all of the variability that occurred. While energetic electron precipitation can be described through a proxy such as Kp or Dst, careful incorporation of time delays for different electron energies must be included. Dst was found to be the most accurate proxy for electron precipitation during the weak recurrent-activity period studied.]]> Sat 24 Mar 2018 08:07:56 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:10988 Sat 24 Mar 2018 08:07:55 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3342 Sat 24 Mar 2018 07:22:35 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3486 Sat 24 Mar 2018 07:20:36 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3444 Sat 24 Mar 2018 07:20:28 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3462 Sat 24 Mar 2018 07:20:27 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3373 Sat 24 Mar 2018 07:18:59 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4824 Sat 24 Mar 2018 07:18:53 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:4853 Sat 24 Mar 2018 07:18:52 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:3176 Sat 24 Mar 2018 07:18:11 AEDT ]]> https://nova.newcastle.edu.au/vital/access/ /manager/Repository/uon:35538 Mon 26 Aug 2019 13:08:06 AEST ]]>