Bibliography
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Found 19 entries in the Bibliography.
Showing entries from 1 through 19
| 2010 |
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Comparison of the Hill\textendashSiscoe polar cap potential theory with the Weimer and AMIE models Kelley, Michael; Crowley, Geoffrey; Weimer, Daniel; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: Jan-03-2010 YEAR: 2010 DOI: 10.1016/j.jastp.2009.02.011 |
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Miller, E.; Makela, J.; Groves, K.; Kelley, M.; Tsunoda, R.; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2009JA014946 |
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Kelley, M.; Nicolls, M.; Varney, R.; Collins, R.; Doe, R.; Plane, J.; Thayer, J.; Taylor, M.; Thurairajah, B.; Mizutani, K.; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2009JA014938 |
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Comparison of the Hill–Siscoe polar cap potential theory with the Weimer and AMIE models The magnetic storm on November 2004 was characterized by a high solar wind pressure and thus offers a unique opportunity to test the Hill–Siscoe formula (H–S) for the polar cap potential (PCP). To estimate the polar cap potential, we use the Weimer Statistical Convection Model (WCM), and the Assimilative Mapping of Ionospheric Electrodynamics Model (AMIE), based on ingestion of a number of data sets. H–S is in excellent agreement with WCM, and with AMIE during times when DMSP is used in the latter. The implication is that the AMIE conductivity model yields conductivities that are too high by a factor of 2–3. Both H–S and WCM display saturation effects, although WCM is more severe. The two methods track well until an IEF of about 20mV/m occurs, where H–S continues to increase while WCM levels off. Even at high electric field values, the pressure increases the denominator of the H–S formula by 60\%, keeping the potential lower than its saturation value. There are several H–S points above 250kV, even up to 400kV, that are not found in WCM and occur right after a rapid transition from Bz north to south. For Bz north, we find evidence for a saturation effect on the PCP at large IEF, little effect as a function of solar wind velocity, and an increase of the PCP with increasing pressure. This seems to rule out viscous interaction but may involve geometric changes in the high-altitude polar cusp that affect recombination there for Bz north. Kelley, Michael; Crowley, Geoffrey; Weimer, Daniel; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: YEAR: 2010 DOI: https://doi.org/10.1016/j.jastp.2009.02.011 Magnetic storm; Polar cap potential; Hill–Siscoe formula; solar wind |
| 2009 |
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We investigate the effects of penetration electric fields, meridional thermospheric neutral winds, and composition perturbation zones (CPZs) on the distribution of low-latitude plasma during the 7\textendash11 November 2004 geomagnetic superstorm. The impact on low-latitude plasma was assessed using total electron content (TEC) measurements from a latitudinally distributed array of ground-based GPS receivers in South America. Jicamarca Radio Observatory incoherent scatter radar measurements of vertical E\texttimesB drift are used in combination with the Low-Latitude IONospheric Sector (LLIONS) model to examine how penetration electric fields and meridional neutral winds shape low-latitude TEC. It is found that superfountain conditions pertain between \~1900 and 2100UT on 9 November, creating enhanced equatorial ionization anomaly (EIA) crests at \textpm20\textdegree geomagnetic latitude. Large-amplitude and/or long-duration changes in the electric field were found to produce significant changes in EIA plasma density and latitudinal location, with a delay time of \~2\textendash2.5h. Superfountain drifts were primarily responsible for EIA TEC levels; meridional winds were needed only to create hemispherical crest TEC asymmetries. The [O/N2] density ratio (derived from the GUVI instrument, flown on the TIMED satellite) and measurements of total atmospheric density (from the GRACE satellites), combined with TEC measurements, yield information regarding a likely CPZ that appeared on 10 November, suppressing TEC for over 16h. Mannucci, Anthony; Tsurutani, Bruce; Kelley, Michael; Iijima, Byron; Komjathy, Attila; Published by: Journal of Geophysical Research Published on: Jan-01-2009 YEAR: 2009 DOI: 10.1029/2009JA014043 |
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Chu, X; Collins, RL; Stevens, MH; Plane, JM; Meier, RR; Deland, MT; Kelley, MC; Nicolls, MJ; Thurairajah, B; Varney, RH; , others; Published by: Published on: |
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On the origin of pre-reversal enhancement of the zonal equatorial electric field Kelley, MC; Ilma, RR; Crowley, G; Published by: Published on: |
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Miller, ES; Comberiate, J; Makela, JJ; Paxton, LJ; Kelley, MC; Groves, KM; Tsunoda, RT; Published by: Published on: |
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Coordinated Ground-and Space-based 3-D Electron Density Reconstruction and Plasma Bubble Imaging Comberiate, J; Miller, ES; Paxton, LJ; Makela, JJ; Kelley, MC; Published by: Published on: |
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Kelley, MC; Seyler, CE; Larsen, MF; Published by: Geophysical Research Letters Published on: |
| 2007 |
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Longitudinal structure of the vertical E$\times$ B drift and ion density seen from ROCSAT-1 Kil, Hyosub; Oh, S-J; Kelley, MC; Paxton, LJ; England, SL; Talaat, E; Min, K-W; Su, S-Y; Published by: Geophysical Research Letters Published on: |
| 2006 |
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Convective ionospheric storms: A major space weather problem Kelley, Michael; Makela, Jonathan; ere, Odile; Published by: Published on: |
| 2003 |
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The first coordinated ground- and space-based optical observations of equatorial plasma bubbles We report on ionospheric optical emissions detected by the GUVI instrument on the TIMED satellite. As the satellite crosses the equatorial zone the bright Appleton Anomaly region is imaged. Often these bright zones are interrupted by regions slanted from west to east as the equator is approached forming a backwards \textquoteleftC\textquoteright-shape in the image. To explain this feature we use simultaneous ground-based observations looking equatorward from Hawaii using the 777.4-nm emission. We also compare these optical observations to inverted electron density maps, as well as to those made by radar and to numerical simulations of the Rayleigh-Taylor instability. The characteristic shape is a result of a shear in the eastward plasma flow velocity, which peaks near the F peak at the equator and decreases both above and below that height. The ability to detect these unstable and usually turbulent ionospheric regions from orbit provides a powerful global remote sensing capability for an important space weather process. Kelley, Michael; Makela, J.; Paxton, L.; Kamalabadi, F.; Comberiate, J.; Kil, H.; Published by: Geophysical Research Letters Published on: 07/2003 YEAR: 2003 DOI: 10.1029/2003GL017301 |
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Study of the Pre-Reversal Enhancement at the Jicamarca Radio Observatory using the ASPEN-TIMEGCM Makela, JJ; Crowley, G; Kelley, MC; Nicolls, MJ; Kudeki, E; Chau, JL; Published by: Published on: |
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Geosynchronous Imaging of the Earth s Ionosphere: Development Phase Under ONR grant N00014-01-1-0702 we explored the value of airglow imagers in the study of the ionosphere. In large part this effort was driven by the need to develop new ways to Published by: Published on: |
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Field-aligned 777.4-nm composite airglow images of equatorial plasma depletions We present a powerful tool to analyze two‐dimensional field‐aligned images of equatorial plasma depletions taken from mid‐latitudes. By shifting each individual image by the sum of Published by: Geophysical Research Letters Published on: |
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The first coordinated ground-and space-based optical observations of equatorial plasma bubbles Kelley, Michael; Makela, Jonathan; Paxton, Larry; Kamalabadi, Farzad; Comberiate, Joseph; Kil, Hyosub; Published by: Geophysical Research Letters Published on: |
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New developments in low and mid-latitude F-region plasma physics Published by: Published on: |
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Establishment of a Patrol Imager at AEOS for Space Weather and Mesospheric Studies Published by: Published on: |
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