https://novaprd-lb.newcastle.edu.au/vital/access/manager/Index ${session.getAttribute("locale")} 5 https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:36226 Wed 11 Mar 2020 11:50:42 AEDT ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:19525 Wed 11 Apr 2018 17:00:38 AEST ]]> https://novaprd-lb.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://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:3260 Wed 11 Apr 2018 15:36:10 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:6846 Wed 11 Apr 2018 15:05:10 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:1993 Wed 11 Apr 2018 14:32:07 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:4836 Wed 11 Apr 2018 11:44:59 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:4834 Wed 11 Apr 2018 10:16:13 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:28883 Wed 11 Apr 2018 09:26:13 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:35008 Thu 30 May 2019 14:44:50 AEST ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:15487 Sat 24 Mar 2018 08:21:27 AEDT ]]> https://novaprd-lb.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://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:11207 Sat 24 Mar 2018 08:12:45 AEDT ]]> https://novaprd-lb.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://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:17429 Sat 24 Mar 2018 08:01:40 AEDT ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:28541 Sat 24 Mar 2018 07:28:47 AEDT ]]> https://novaprd-lb.newcastle.edu.au/vital/access/manager/Repository/uon:22668 Sat 24 Mar 2018 07:12:10 AEDT ]]>