Auroral Zone Ionospheric Considerations for WADGPS

Skone, S.; Cannon, M. Elizabeth

doi:10.1002/j.2161-4296.1998.tb02376.x

Cited by 8 publications

(5 citation statements)

References 14 publications

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“…Nightside discrete auroras are likely to produce larger TEC variations and to occur more frequently. The limited spatial extent and fast temporal behavior of the auroral TEC perturbations suggests that differentially aided or augmented GPS systems will not be able to practically correct for these error sources [ Skone and Cannon , 1998].…”

Section: Discussionmentioning

confidence: 99%

Simultaneous total electron content and all‐sky camera measurements of an auroral arc

et al. 2002

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[1] We present an example of Global Positioning System (GPS) derived total electron content (TEC) and all-sky camera (ASC) images that show increases of TEC by $10 Â 10 16 electrons m À2 (10 TEC units) occurring simultaneously with auroral light in ASC images. The TEC example appears to be an E region density enhancement produced by two discrete auroral arcs occurring in the late morning auroral oval at 1000 LT. This suggests that GPS signal TEC measurements can be used to detect individual auroral arcs and that individual discrete auroral arcs are responsible for some high-latitude phase scintillations. The specific auroral feature detected was a poleward moving auroral form believed to occur in the polar cap where the ionosphere is convecting antisunward. The magnitude of the rate of change of TEC (dTEC/dt) is comparable to that previously reported. However, the timescales associated with the event, the order of 1 min, suggest that the data sampling technique commonly used by chain GPS TEC receivers (averaging and time decimation) will undersample E region TEC perturbations produced by active auroral displays. The localized nature of this example implies that L1 ranging errors of at least 1.6 m will be introduced by auroral arcs into systems relying on differential GPS for navigation or augmentation. Although the TEC and auroral arcs presented herein occurred in the late morning auroral oval, we expect that the effects of discrete auroral arcs on GPS TEC and subsequent ranging errors should occur at all local times. Furthermore, GPS receivers can be used to detect individual discrete arcs.

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Section: Discussionmentioning

confidence: 99%

Simultaneous total electron content and all‐sky camera measurements of an auroral arc

et al. 2002

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“…Dependence of scintillation intensity on solar and geomagnetic activity, as well as season and local time has been recognized for many years (Aarons, 1982). Geomagnetic activity is often used as a convenient proxy to characterize the ionospheric conditions and a clear dependence of temporal and spatial variability of TEC on ionospheric activity has been demonstrated (e.g., Skone et al, 1998). Although scintillation is most intense at low latitudes (Aarons, 1982;Basu et al, 2002) it can be strong in high latitudes during disturbed conditions (Doherty et al, 2004).…”

Section: Introductionmentioning

confidence: 99%

GPS TEC, scintillation and cycle slips observed at high latitudes during solar minimum

et al. 2010

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Abstract. High-latitude irregularities can impair the operation of GPS-based devices by causing fluctuations of GPS signal amplitude and phase, also known as scintillation. Severe scintillation events lead to losses of phase lock, which result in cycle slips. We have used data from the Canadian High Arctic Ionospheric Network (CHAIN) to measure amplitude and phase scintillation from L1 GPS signals and total electron content (TEC) from L1 and L2 GPS signals to study the relative role that various high-latitude irregularity generation mechanisms have in producing scintillation. In the first year of operation during the current solar minimum the amplitude scintillation has remained very low but events of strong phase scintillation have been observed. We have found, as expected, that auroral arc and substorm intensifications as well as cusp region dynamics are strong sources of phase scintillation and potential cycle slips. In addition, we have found clear seasonal and universal time dependencies of TEC and phase scintillation over the polar cap region. A comparison with radio instruments from the Canadian GeoSpace Monitoring (CGSM) network strongly suggests that the polar cap scintillation and TEC variations are associated with polar cap patches which we therefore infer to be main contributors to scintillation-causing irregularities in the polar cap.

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“…At high latitudes, ionospheric irregularities occur in association with auroral activities (Aarons et al., 1995; Pi et al., 1997; Pryse et al., 1996) and are activated by auroral particle precipitation and the dynamic processes of high‐speed plasma convection (Fejer & Kelley, 1980; Keskinen & Ossakow, 1983; Phelps & Sagalyn, 1976). These irregularities cause phase and amplitude fluctuations in global navigation satellite system (GNSS) signals and have been extensively investigated using ground‐based GNSS data (Alfonsi et al., 2011; Cherniak et al., 2014; Cherniak & Zakharenkova, 2016; Jacobsen & Andalsvik, 2016; Jiao et al., 2013; Mitchell et al., 2005; Prikryl et al., 2013, 2014; Skone & Cannon, 1998; Tiwari et al., 2013; Watson et al., 2011). In contrast, plasma bubbles, which are characterized by plasma density depletion, often appear after sunset in low‐latitude and equatorial regions of the ionosphere, and contain plasma density irregularities within them.…”

Section: Introductionmentioning

confidence: 99%

Dependence of Ionospheric Responses on Solar Wind Dynamic Pressure During Geomagnetic Storms Using Global Long‐Term GNSS‐TEC Data

et al. 2023

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The arrival of a strong southward interplanetary magnetic field (IMF) at the dayside magnetopause enhances the magnetospheric convection associated with the merging of the southward IMF and Earth's magnetic field, which transports hot plasma sheet particles into the inner magnetosphere and forms a ring current that depresses the H-component of the geomagnetic field at mid-and low-latitudes. This magnetic signature is known as a geomagnetic storm. Furthermore, a part of the injected plasma sheet particles is carried along the magnetic field lines and precipitated into the atmosphere at the auroral zone as high-energy particle precipitation, resulting in auroral oval emissions (

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Auroral Zone Ionospheric Considerations for WADGPS

Cited by 8 publications

References 14 publications

Simultaneous total electron content and all‐sky camera measurements of an auroral arc

Simultaneous total electron content and all‐sky camera measurements of an auroral arc

GPS TEC, scintillation and cycle slips observed at high latitudes during solar minimum

Dependence of Ionospheric Responses on Solar Wind Dynamic Pressure During Geomagnetic Storms Using Global Long‐Term GNSS‐TEC Data

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