GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 2: Interhemispheric comparison

Prikryl, P.; Ghoddousi‐Fard, Reza; Spogli, Luca; Mitchell, Cathryn N.; Li, G.; Ning, Baiqi; Cilliers, Pierre J.; Sreeja, V.; Aquino, Márcio; Terkildsen, M.; Jayachandran, P. T.; Jiao, Yu; Morton, Yu; Ruohoniemi, J. M.; Thomas, E. G.; Zhang, Yongliang; Weatherwax, A. T.; Alfonsi, Lucilla; Franceschi, Giorgiana De; Romano, Vincenzo

doi:10.5194/angeo-33-657-2015

Cited by 17 publications

(12 citation statements)

References 62 publications

(74 reference statements)

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“…There is a possibility of SAPSs at the equatorward edge of the return flow just poleward of the main trough as it was in the case reported by Makarevich and Bristow (2014). During the same event, the SAPS was collocated with a weak scintillation (sDPR < 5 mm s −1 ) (Prikryl et al, 2015b) (further discussed below). Figure 7c shows a 5 min mean TEC map overlaid with the electrostatic potential contours and scintillation IPPs.…”

Section: Event S1: 7 March 2012 -Case Of Imf B Z <mentioning

confidence: 76%

“…2). SuperDARN observations of SAPSs were previously associated with weak phase scintillation that mapped along the equatorward border of the auroral oval (Prikryl et al, 2013b(Prikryl et al, , 2015b. During storm S1, weak scintillation IPPs scintillation mapped to the poleward edge of the main trough (Fig.…”

Section: Discussionmentioning

confidence: 92%

“…They included intense, sometimes pulsed, flows in the cusp, which are the ionospheric signatures of magnetic reconnection between the southward IMF and the northward Earth magnetic field at the dayside magnetopause. These ionospheric flows can have a large extent in longitude and lead to an overall intensification of the dayside convection in the dawn or dusk cells, depending on the IMF B y polarity that controls the dawn-dusk asymmetry of the ionospheric convection pattern (Ruohoniemi and Greenwald, 2005;Grocott et al, 2010). This is further addressed in the companion paper (Prikryl et al, 2015a).…”

Section: Discussionmentioning

confidence: 94%

“…org) with the TEC data downloaded from the Madrigal database (http://madrigal.haystack.mit.edu/madrigal/). The TEC data were processed using MIT Automated Processing of GPS (MAPGPS) software, which allows the processing of GPS data into global TEC maps (Rideout and Coster, 2006). Solar wind data were obtained from the Goddard Space Flight Center Space Physics Data Facility CDAWeb and OMNIWeb data sets (King and Papitashvili, 2005).…”

Section: Instruments and Datamentioning

confidence: 99%

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GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 1: The North American sector

et al. 2015

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Abstract. The interval of geomagnetic storms of 7-17 March 2012 was selected at the Climate and Weather of the Sun-Earth System (CAWSES) II Workshop for group study of space weather effects during the ascending phase of solar cycle 24 (Tsurutani et al., 2014). The high-latitude ionospheric response to a series of storms is studied using arrays of GPS receivers, HF radars, ionosondes, riometers, magnetometers, and auroral imagers focusing on GPS phase scintillation. Four geomagnetic storms showed varied responses to solar wind conditions characterized by the interplanetary magnetic field (IMF) and solar wind dynamic pressure. As a function of magnetic latitude and magnetic local time, regions of enhanced scintillation are identified in the context of coupling processes between the solar wind and the magnetosphere-ionosphere system. Large southward IMF and high solar wind dynamic pressure resulted in the strongest scintillation in the nightside auroral oval. Scintillation occurrence was correlated with ground magnetic field perturbations and riometer absorption enhancements, and collocated with mapped auroral emission. During periods of southward IMF, scintillation was also collocated with ionospheric convection in the expanded dawn and dusk cells, with the antisunward convection in the polar cap and with a tongue of ionization fractured into patches. In contrast, large northward IMF combined with a strong solar wind dynamic pressure pulse was followed by scintillation caused by transpolar arcs in the polar cap.

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Section: Event S1: 7 March 2012 -Case Of Imf B Z <mentioning

confidence: 76%

Section: Discussionmentioning

confidence: 92%

Section: Discussionmentioning

confidence: 94%

Section: Instruments and Datamentioning

confidence: 99%

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GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 1: The North American sector

et al. 2015

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“…This difference in the ionospheric response can be explained by interhemispheric asymmetry due to the high-latitude coupling between solar wind and the magnetosphere. This asymmetry drives the dawn-dusk component of the interplanetary magnetic field that defines the cusp location and thus determines whether the stormenhanced density plasma will enter the polar cap and the orientation of the antisunward convection in the polar cap relative to the noon-midnight meridian (Cherniak et al, 2015;Horvarth and Lovell, 2015;Prikryl et al, 2013Prikryl et al, , 2015b.…”

Section: Discussionmentioning

confidence: 99%

Ionospheric F-region response to the 26 September 2011 geomagnetic storm in the Antarctica American and Australian sectors

et al. 2017

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Abstract. The ionospheric response at middle and high latitudes in the Antarctica American and Australian sectors to the 26-27 September 2011 moderately intense geomagnetic storm was investigated using instruments including an ionosonde, riometer, and GNSS receivers. The multiinstrument observations permitted us to characterize the ionospheric storm-enhanced density (SED) and tongues of ionization (TOIs) as a function of storm time and location, considering the effect of prompt penetration electric fields (PPEFs). During the main phase of the geomagnetic storm, dayside SEDs were observed at middle latitudes, and in the nightside only density depletions were observed from middle to high latitudes. Both the increase and decrease in ionospheric density at middle latitudes can be attributed to a combination of processes, including the PPEF effect just after the storm onset, dominated by disturbance dynamo processes during the evolution of the main phase. Two SEDs-TOIs were identified in the Southern Hemisphere, but only the first episode had a counterpart in the Northern Hemisphere. This difference can be explained by the interhemispheric asymmetry caused by the high-latitude coupling between solar wind and the magnetosphere, which drives the dawn-to-dusk component of the interplanetary magnetic field. The formation of polar TOI is a function of the SED plume location that might be near the dayside cusp from which it can enter the polar cap, which was the case in the Southern Hemisphere. Strong GNSS scintillations were observed at stations collocated with SED plumes at middle latitudes and cusp on the dayside and at polar cap TOIs on the nightside.

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Satellite‐beacon Ionospheric‐scintillation Global Model of the upper Atmosphere (SIGMA) II: Inverse modeling with high‐latitude observations to deduce irregularity physics

et al. 2016

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Ionospheric scintillation is caused by irregularities in the ionospheric electron density. The characterization of ionospheric irregularities is important to further our understanding of the underlying physics. Our goal is to characterize the intermediate (0.1–10 km) to medium (10–100 km) scale high‐latitude irregularities which are likely to produce these scintillations. In this paper, we characterize irregularities observed by Global Navigation Satellite System (GNSS) during a geomagnetically active period on 9 March 2012. For this purpose, along with the measurements, we are using the recently developed model: “Satellite‐beacon Ionospheric‐scintillation Global Model of the upper Atmosphere” (SIGMA). The model is particularly applicable at high latitudes as it accounts for the complicated geometry of the magnetic field lines in these regions and is presented in an earlier paper. We use an inverse modeling technique to derive irregularity parameters by comparing the high rate (50 Hz) GNSS observations to the modeled outputs. In this investigation, we consider experimental observations from both the northern and southern high latitudes. The results include predominance of phase scintillations compared to amplitude scintillations that imply the presence of larger‐scale irregularities of sizes above the Fresnel scale at GPS frequencies, and the spectral index ranges from 2.4 to 4.2 and the RMS number density ranges from 3e11 to 2.3e12 el/m3. The best fits we obtained from our inverse method that considers only weak scattering mostly agree with the observations. Finally, we suggest some improvements in order to facilitate the possibility of accomplishing a unique solution to such inverse problems.

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GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 2: Interhemispheric comparison

Cited by 17 publications

References 62 publications

GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 1: The North American sector

GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 1: The North American sector

Ionospheric F-region response to the 26 September 2011 geomagnetic storm in the Antarctica American and Australian sectors

Satellite‐beacon Ionospheric‐scintillation Global Model of the upper Atmosphere (SIGMA) II: Inverse modeling with high‐latitude observations to deduce irregularity physics

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