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Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010

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Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010. / Prikryl, P.; Spogli, L.; Jayachandran, P. T. et al.
In: Annales Geophysicae, Vol. 29, No. 12, 21.12.2011, p. 2287-2304.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Prikryl, P, Spogli, L, Jayachandran, PT, Kinrade, J, Mitchell, CN, Ning, B, Li, G, Cilliers, PJ, Terkildsen, M, Danskin, DW, Spanswick, E, Donovan, E, Weatherwax, AT, Bristow, WA, Alfonsi, L, De Franceschi, G, Romano, V, Ngwira, CM & Opperman, BDL 2011, 'Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010', Annales Geophysicae, vol. 29, no. 12, pp. 2287-2304. https://doi.org/10.5194/angeo-29-2287-2011

APA

Prikryl, P., Spogli, L., Jayachandran, P. T., Kinrade, J., Mitchell, C. N., Ning, B., Li, G., Cilliers, P. J., Terkildsen, M., Danskin, D. W., Spanswick, E., Donovan, E., Weatherwax, A. T., Bristow, W. A., Alfonsi, L., De Franceschi, G., Romano, V., Ngwira, C. M., & Opperman, B. D. L. (2011). Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010. Annales Geophysicae, 29(12), 2287-2304. https://doi.org/10.5194/angeo-29-2287-2011

Vancouver

Prikryl P, Spogli L, Jayachandran PT, Kinrade J, Mitchell CN, Ning B et al. Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010. Annales Geophysicae. 2011 Dec 21;29(12):2287-2304. doi: 10.5194/angeo-29-2287-2011

Author

Prikryl, P. ; Spogli, L. ; Jayachandran, P. T. et al. / Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010. In: Annales Geophysicae. 2011 ; Vol. 29, No. 12. pp. 2287-2304.

Bibtex

@article{03cffc3084e648f4b007e36e31e6b1e1,
title = "Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010",
abstract = "Arrays of GPS Ionospheric Scintillation and TEC Monitors (GISTMs) are used in a comparative scintillation study focusing on quasi-conjugate pairs of GPS receivers in the Arctic and Antarctic. Intense GPS phase scintillation and rapid variations in ionospheric total electron content (TEC) that can result in cycle slips were observed at high latitudes with dual-frequency GPS receivers during the first significant geomagnetic storm of solar cycle 24 on 5-7 April 2010. The impact of a bipolar magnetic cloud of north-south (NS) type embedded in high speed solar wind from a coronal hole caused a geomagnetic storm with maximum 3-hourly Kp = 8- and hourly ring current Dst = -73 nT. The interhemispheric comparison of phase scintillation reveals similarities but also asymmetries of the ionospheric response in the northern and southern auroral zones, cusps and polar caps. In the nightside auroral oval and in the cusp/cleft sectors the phase scintillation was observed in both hemispheres at about the same times and was correlated with geomagnetic activity. The scintillation level was very similar in approximately conjugate locations in Qiqiktarjuaq (75.4 degrees N; 23.4 degrees E CGM lat. and lon.) and South Pole (74.1 degrees S; 18.9 degrees E), in Longyearbyen (75.3 degrees N; 111.2 degrees E) and Zhongshan (74.7 degrees S; 96.7 degrees E), while it was significantly higher in Cambridge Bay (77.0 degrees N; 310.1 degrees E) than at Mario Zucchelli (80.0 degrees S; 307.7 degrees E). In the polar cap, when the interplanetary magnetic field (IMF) was strongly northward, the ionization due to energetic particle precipitation was a likely cause of scintillation that was stronger at Concordia (88.8 degrees S; 54.4 degrees E) in the dark ionosphere than in the sunlit ionosphere over Eureka (88.1 degrees N; 333.4 degrees E), due to a difference in ionospheric conductivity. When the IMF tilted southward, weak or no significant scintillation was detected in the northern polar cap, while in the southern polar cap rapidly varying TEC and strong phase scintillation persisted for many hours. This interhemispheric asymmetry is explained by the difference in the location of solar terminator relative to the cusps in the Northern and Southern Hemisphere. Solar terminator was in the immediate proximity of the cusp in the Southern Hemisphere where sunlit ionospheric plasma was readily convected into the central polar cap and a long series of patches was observed. In contrast, solar terminator was far poleward of the northern cusp thus reducing the entry of sunlit plasma and formation of dense patches. This is consistent with the observed and modeled seasonal variation in occurrence of polar cap patches. The GPS scintillation and TEC data analysis is supported by data from ground- based networks of magnetometers, riometers, ionosondes, HF radars and all- sky imagers, as well as particle flux measurements by DMSP satellites.",
keywords = "Ionosphere, Ionospheric irregularities, Magnetospheric physics, Storms and substorms, Radio science, Space and satellite communication, DENSITY STRUCTURES, SOLAR MINIMUM, POLAR IONOSPHERE, AURORAL OVAL, JANUARY 10, GEOEFFECTIVENESS, DYNAMICS, PATCHES, FLUCTUATIONS, CLIMATOLOGY",
author = "P. Prikryl and L. Spogli and Jayachandran, {P. T.} and J. Kinrade and Mitchell, {C. N.} and B. Ning and G. Li and Cilliers, {P. J.} and M. Terkildsen and Danskin, {D. W.} and E. Spanswick and E. Donovan and Weatherwax, {A. T.} and Bristow, {W. A.} and L. Alfonsi and {De Franceschi}, G. and V. Romano and Ngwira, {C. M.} and Opperman, {B. D. L.}",
year = "2011",
month = dec,
day = "21",
doi = "10.5194/angeo-29-2287-2011",
language = "English",
volume = "29",
pages = "2287--2304",
journal = "Annales Geophysicae",
issn = "0992-7689",
publisher = "European Geosciences Union",
number = "12",

}

RIS

TY - JOUR

T1 - Interhemispheric comparison of GPS phase scintillation at high latitudes during the magnetic-cloud-induced geomagnetic storm of 5-7 April 2010

AU - Prikryl, P.

AU - Spogli, L.

AU - Jayachandran, P. T.

AU - Kinrade, J.

AU - Mitchell, C. N.

AU - Ning, B.

AU - Li, G.

AU - Cilliers, P. J.

AU - Terkildsen, M.

AU - Danskin, D. W.

AU - Spanswick, E.

AU - Donovan, E.

AU - Weatherwax, A. T.

AU - Bristow, W. A.

AU - Alfonsi, L.

AU - De Franceschi, G.

AU - Romano, V.

AU - Ngwira, C. M.

AU - Opperman, B. D. L.

PY - 2011/12/21

Y1 - 2011/12/21

N2 - Arrays of GPS Ionospheric Scintillation and TEC Monitors (GISTMs) are used in a comparative scintillation study focusing on quasi-conjugate pairs of GPS receivers in the Arctic and Antarctic. Intense GPS phase scintillation and rapid variations in ionospheric total electron content (TEC) that can result in cycle slips were observed at high latitudes with dual-frequency GPS receivers during the first significant geomagnetic storm of solar cycle 24 on 5-7 April 2010. The impact of a bipolar magnetic cloud of north-south (NS) type embedded in high speed solar wind from a coronal hole caused a geomagnetic storm with maximum 3-hourly Kp = 8- and hourly ring current Dst = -73 nT. The interhemispheric comparison of phase scintillation reveals similarities but also asymmetries of the ionospheric response in the northern and southern auroral zones, cusps and polar caps. In the nightside auroral oval and in the cusp/cleft sectors the phase scintillation was observed in both hemispheres at about the same times and was correlated with geomagnetic activity. The scintillation level was very similar in approximately conjugate locations in Qiqiktarjuaq (75.4 degrees N; 23.4 degrees E CGM lat. and lon.) and South Pole (74.1 degrees S; 18.9 degrees E), in Longyearbyen (75.3 degrees N; 111.2 degrees E) and Zhongshan (74.7 degrees S; 96.7 degrees E), while it was significantly higher in Cambridge Bay (77.0 degrees N; 310.1 degrees E) than at Mario Zucchelli (80.0 degrees S; 307.7 degrees E). In the polar cap, when the interplanetary magnetic field (IMF) was strongly northward, the ionization due to energetic particle precipitation was a likely cause of scintillation that was stronger at Concordia (88.8 degrees S; 54.4 degrees E) in the dark ionosphere than in the sunlit ionosphere over Eureka (88.1 degrees N; 333.4 degrees E), due to a difference in ionospheric conductivity. When the IMF tilted southward, weak or no significant scintillation was detected in the northern polar cap, while in the southern polar cap rapidly varying TEC and strong phase scintillation persisted for many hours. This interhemispheric asymmetry is explained by the difference in the location of solar terminator relative to the cusps in the Northern and Southern Hemisphere. Solar terminator was in the immediate proximity of the cusp in the Southern Hemisphere where sunlit ionospheric plasma was readily convected into the central polar cap and a long series of patches was observed. In contrast, solar terminator was far poleward of the northern cusp thus reducing the entry of sunlit plasma and formation of dense patches. This is consistent with the observed and modeled seasonal variation in occurrence of polar cap patches. The GPS scintillation and TEC data analysis is supported by data from ground- based networks of magnetometers, riometers, ionosondes, HF radars and all- sky imagers, as well as particle flux measurements by DMSP satellites.

AB - Arrays of GPS Ionospheric Scintillation and TEC Monitors (GISTMs) are used in a comparative scintillation study focusing on quasi-conjugate pairs of GPS receivers in the Arctic and Antarctic. Intense GPS phase scintillation and rapid variations in ionospheric total electron content (TEC) that can result in cycle slips were observed at high latitudes with dual-frequency GPS receivers during the first significant geomagnetic storm of solar cycle 24 on 5-7 April 2010. The impact of a bipolar magnetic cloud of north-south (NS) type embedded in high speed solar wind from a coronal hole caused a geomagnetic storm with maximum 3-hourly Kp = 8- and hourly ring current Dst = -73 nT. The interhemispheric comparison of phase scintillation reveals similarities but also asymmetries of the ionospheric response in the northern and southern auroral zones, cusps and polar caps. In the nightside auroral oval and in the cusp/cleft sectors the phase scintillation was observed in both hemispheres at about the same times and was correlated with geomagnetic activity. The scintillation level was very similar in approximately conjugate locations in Qiqiktarjuaq (75.4 degrees N; 23.4 degrees E CGM lat. and lon.) and South Pole (74.1 degrees S; 18.9 degrees E), in Longyearbyen (75.3 degrees N; 111.2 degrees E) and Zhongshan (74.7 degrees S; 96.7 degrees E), while it was significantly higher in Cambridge Bay (77.0 degrees N; 310.1 degrees E) than at Mario Zucchelli (80.0 degrees S; 307.7 degrees E). In the polar cap, when the interplanetary magnetic field (IMF) was strongly northward, the ionization due to energetic particle precipitation was a likely cause of scintillation that was stronger at Concordia (88.8 degrees S; 54.4 degrees E) in the dark ionosphere than in the sunlit ionosphere over Eureka (88.1 degrees N; 333.4 degrees E), due to a difference in ionospheric conductivity. When the IMF tilted southward, weak or no significant scintillation was detected in the northern polar cap, while in the southern polar cap rapidly varying TEC and strong phase scintillation persisted for many hours. This interhemispheric asymmetry is explained by the difference in the location of solar terminator relative to the cusps in the Northern and Southern Hemisphere. Solar terminator was in the immediate proximity of the cusp in the Southern Hemisphere where sunlit ionospheric plasma was readily convected into the central polar cap and a long series of patches was observed. In contrast, solar terminator was far poleward of the northern cusp thus reducing the entry of sunlit plasma and formation of dense patches. This is consistent with the observed and modeled seasonal variation in occurrence of polar cap patches. The GPS scintillation and TEC data analysis is supported by data from ground- based networks of magnetometers, riometers, ionosondes, HF radars and all- sky imagers, as well as particle flux measurements by DMSP satellites.

KW - Ionosphere

KW - Ionospheric irregularities

KW - Magnetospheric physics

KW - Storms and substorms

KW - Radio science

KW - Space and satellite communication

KW - DENSITY STRUCTURES

KW - SOLAR MINIMUM

KW - POLAR IONOSPHERE

KW - AURORAL OVAL

KW - JANUARY 10

KW - GEOEFFECTIVENESS

KW - DYNAMICS

KW - PATCHES

KW - FLUCTUATIONS

KW - CLIMATOLOGY

U2 - 10.5194/angeo-29-2287-2011

DO - 10.5194/angeo-29-2287-2011

M3 - Journal article

VL - 29

SP - 2287

EP - 2304

JO - Annales Geophysicae

JF - Annales Geophysicae

SN - 0992-7689

IS - 12

ER -