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Reinisch, B. W.; Haines, D. M.; Bibl, K.; Cheney, G.; Galkin, I. A.; Huang, Xin; Myers, S. H.; Sales, Gary S.; Benson, Robert F.; Fung, S. F.; Green, J.L.; Boardsen, S. A.; Taylor, William W.; Bougeret, J.‐L.; Manning, Robert M.; Meyer‐Vernet, N.; Moncuquet, M.; Carpenter, D. L.; Gallagher, D. L.; Reiff, P. H.

doi:10.1023/a:1005252602159

Cited by 141 publications

(22 citation statements)

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“…Krall et al [2014] find that thermospheric winds must be included in order to represent observed asymmetric plasmaspheric azimuthal structure in the equatorial plane, yet this also results in lower refilling rates than without these winds. Rough agreement is found with IMAGE Radio Plasma Imager (RPI) observations [Reinisch, 2000;Denton et al, 2012; see also Tu et al, 2003;Reinisch et al, 2004;Tu et al, 2006;Fu et al, 2010], but those comparisons are limited in time and magnetic local time. The SAMI3 refilling rates are smaller than those observed by RPI at low L value and higher at higher L, as given by their and our equation (1)…”

Section: State Of Modeled Refillingsupporting

confidence: 57%

Unsolved problems in plasmasphere refilling

Gallagher

Comfort

2016

JGR Space Physics

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The plasmasphere is a cold (~1 eV) plasma at middle to low magnetic latitudes surrounding the Earth. Its shape is dominated by Earth's magnetic field and its cross‐field motion is dominated by electric fields. It is a highly coupled part of the inner magnetosphere. Storm time conditions erode the outer plasmasphere, transporting that plasma into the dayside magnetosheath region, leaving behind a region of greatly reduced plasma density that will refill from ionospheric outflow. The processes involved in refilling remain incompletely understood. In this commentary, outstanding questions about plasmaspheric refilling are summarized in the context of recent publications.

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Section: State Of Modeled Refillingsupporting

confidence: 57%

Unsolved problems in plasmasphere refilling

Gallagher

Comfort

2016

JGR Space Physics

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“…In SAMI3, thermospheric composition and wind information are typically specified using empirical models, such as the MSIS ® atmosphere model (MSIS is named for the mass spectrometer and incoherent scatter data upon which it was originally based; it was later extended to the exosphere) and the HWM (Horizontal Wind Model). Krall et al [2014] obtained good agreement between SAMI3 and in situ electron density measurements during 1-5 February 2011 using the Naval Research Laboratory MSIS Extended model NRLMSISE-00 [Picone et al, 2002] for composition and HWM07 [Drob et al, 2008] for winds. Krall et al [2016] further demonstrated that refilling rates are sensitive to thermospheric neutral O density and that a reduction of NRLMSISE-00 O density values (by 20%) and in temperature values above 600 km (by 20%) produced reasonable agreement between SAMI3 and in situ electron densities measured during the quiet poststorm period from 25 November to 1 December 2001.…”

Section: Introductionmentioning

confidence: 80%

Day‐to‐day variability in the thermosphere and its impact on plasmasphere refilling

et al. 2016

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Satellite drag data showing significant (20%) short‐term variations in atmospheric mass density are presented. These data, along with the Naval Research Laboratory SAMI3 (Sami3 is Also a Model of the Ionosphere) ionosphere/plasmasphere model and the WACCM (Whole Atmosphere Community Climate Model) atmosphere model are used to estimate day‐to‐day variability in thermosphere composition, thermosphere winds, and exosphere temperatures and the effect of this variability on plasmasphere refilling rates. This assessment is guided by SAMI3 modeling showing that modest (20%) decreases in thermospheric density and exospheric temperature can lead to large (60%) increases in plasmaspheric refilling rates and that changes in the thermospheric wind pattern can have a similar effect. Results suggest that day‐to‐day variability in thermospheric wind and composition could affect plasmaspheric refilling rates by 50 to 100%.

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“…Measurements of n e in the inner magnetosphere are available from Radio Plasma Imager (RPI) instrument [Reinisch, 2000] on the IMAGE spacecraft, operating in the passive mode. During the November event IMAGE passes through the plasmasphere were close to 0845 and 2040 magnetic local time (MLT) at intervals of about 14 h. During the February event, passes were at MLT 0345 and 1545.…”

Section: Image/rpi Electron Densitymentioning

confidence: 99%

Measurement and modeling of the refilling plasmasphere during 2001

et al. 2016

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The Naval Research Laboratory SAMI3 (Sami3 is Also a Model of the Ionosphere) and the RAM‐CPL (Ring current Atmosphere interaction Model‐Cold PLasma) codes are used to model observed plasmasphere dynamics during 25 November 2001 to 1 December 2001 and 1–5 February 2001. Model results compare well to plasmasphere observations of electron and mass densities. Comparison of model results to refilling data and to each other shows good agreement, generally within a factor of 2. We find that SAMI3 plasmaspheric refilling rates and ion densities are sensitive to the composition and temperature of the thermosphere and exosphere, and to photoelectron heating. Results also support our previous finding that the wind‐driven dynamo significantly impacts both refilling rates and plasmasphere dynamics during quiet periods.

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Cited by 141 publications

References 0 publications

Unsolved problems in plasmasphere refilling

Unsolved problems in plasmasphere refilling

Day‐to‐day variability in the thermosphere and its impact on plasmasphere refilling

Measurement and modeling of the refilling plasmasphere during 2001

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