A comprehensive analysis of the geomagnetic storms occurred during 18 February and 2 March 2014

Ghamry, Essam; Lethy, Ahmed; Arafa-Hamed, Tareq; Elaal, Esmat Abd

doi:10.1016/j.nrjag.2016.03.001

Cited by 16 publications

(16 citation statements)

References 41 publications

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“…AE indicates the strength of the auroral electrojet, and it increases when the B z and Dst begins to decrease around 14:00 UTC on 18 February. The solar wind proton density also shows activity at this time, ~10 cm −3 , and then it diminishes and only shows increased values again when the first CME impacts [ Ghamry et al ., ]. Station Sisimiut (SISI) can be under either the polar cap or the auroral oval, depending on geomagnetic and storm conditions.…”

Section: Methods Instrumentation and Observationsmentioning

confidence: 99%

“…The storm was highly complex and had multiple main and recovery phases resulting from a series of Earthdirected CMEs (see http://geomag.usgs.gov/storm/storm18.php and Ghamry et al [2016] for details). As shown in section 2, Dst, AE, and PCN are all geomagnetic indices but there are also fundamental differences among them.…”

Section: Analysis Of Solar Wind Parameters and Geomagnetic Observationsmentioning

confidence: 99%

“…After that time all stations exhibit negative storm effects with diminished TEC values for several days. For a comprehensive analysis of the solar wind parameters during the 19 February 2014 storm seeGhamry et al [2016].…”

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confidence: 99%

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Multiinstrument observations of a geomagnetic storm and its effects on the Arctic ionosphere: A case study of the 19 February 2014 storm

et al. 2017

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We present a multiinstrumented approach for the analysis of the Arctic ionosphere during the 19 February 2014 highly complex, multiphase geomagnetic storm, which had the largest impact on the disturbance storm‐time index that year. The geomagnetic storm was the result of two powerful Earth‐directed coronal mass ejections (CMEs). It produced a strong long lasting negative storm phase over Greenland with a dominant energy input in the polar cap. We employed global navigation satellite system (GNSS) networks, geomagnetic observatories, and a specific ionosonde station in Greenland. We complemented the approach with spaceborne measurements in order to map the state and variability of the Arctic ionosphere. In situ observations from the Canadian CASSIOPE (CAScade, Smallsat and IOnospheric Polar Explorer) satellite's ion mass spectrometer were used to derive ion flow data from the polar cap topside ionosphere during the event. Our research specifically found that (1) thermospheric O/N2 measurements demonstrated significantly lower values over the Greenland sector than prior to the storm time. (2) An increased ion flow in the topside ionosphere was observed during the negative storm phase. (3) Negative storm phase was a direct consequence of energy input into the polar cap. (4) Polar patch formation was significantly decreased during the negative storm phase. This paper addresses the physical processes that can be responsible for this ionospheric storm development in the northern high latitudes. We conclude that ionospheric heating due to the CME's energy input caused changes in the polar atmosphere resulting in Ne upwelling, which was the major factor in high‐latitude ionosphere dynamics for this storm.

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Section: Methods Instrumentation and Observationsmentioning

confidence: 99%

Section: Analysis Of Solar Wind Parameters and Geomagnetic Observationsmentioning

confidence: 99%

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Multiinstrument observations of a geomagnetic storm and its effects on the Arctic ionosphere: A case study of the 19 February 2014 storm

et al. 2017

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“…Figure 5iv, a-d and v, a-d respectively show the temporal variation of the Dst and z component of interplanetary magnetic field (IMF B z ) during the storm periods. The storm observed during 17-21 February was highly complex and had multiple main and recovery phases resulting from a series of Earth-directed coronal mass ejections (CMEs) (see Ghamry et al, 2016, for details). The intense storm of 17 February started with sudden storm commencement (SSC) at 09:00 UT.…”

Section: Relation Between the Equatorial Electric Fieldmentioning

confidence: 99%

Investigation of the relationship between the spatial gradient of total electron content (TEC) between two nearby stations and the occurrence of ionospheric irregularities

2019

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Abstract. The relation between the occurrence of ionospheric irregularities and the spatial gradient of total electron content (TEC) derived from two closely located stations (ASAB: 4.34∘ N, 114.39∘ E and DEBK: 3.71∘ N, 109.34∘ E, geomagnetic), located within the equatorial region, over Ethiopia, during the postsunset hours was investigated. In this study, the Global Positioning System (GPS)-derived TEC during the year 2014 obtained from the two stations were employed to investigate the relationship between the gradient of TEC and occurrence of ionospheric irregularities. The spatial gradient of TEC (ΔTEC∕Δlong) and its standard deviation over 15 min, σ(ΔTEC∕Δlong), were used in this study. The rate of change of TEC-derived indices (ROTI, ROTIave) were also utilized. Our results revealed that most of the maximum enhancement and reduction values in ΔTEC∕Δlong are noticeable during the time period between 19:00 and 24:00 LT. In some cases, the peak values in the spatial gradient of TEC are also observed during daytime and postmidnight hours. The intensity level of σ(ΔTEC∕Δlong) observed after postsunset show similar trends with ROTIave, and was stronger (weaker) during equinoctial (solstice) months. The observed enhancement of σ(ΔTEC∕Δlong) in the equinoctial season shows an equinoctial asymmetry where the March equinox was greater than the September equinox. During the postsunset period, the relation between the spatial gradient of TEC obtained from two closely located Global Navigation Satellite System (GNSS) receivers and the equatorial electric field (EEF) was observed. The variation in the gradient of TEC and ROTIave observed during the evening time period show similar trends with EEF with a delay of about 1–2 h between them. The relationship between σ(ΔTEC∕Δlong) and ROTIave correlate linearly with correlation coefficient of C=0.7975 and C=0.7915 over ASAB and DEBK, respectively. The majority of the maximum enhancement and reduction in the spatial gradient of TEC observed during the evening time period may be associated with ionospheric irregularities or equatorial plasma bubbles. In addition to latitudinal gradients, the longitudinal gradient of TEC has contributed significantly to the TEC fluctuations.

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“…These waves are excited by processes at different distances in the magnetosphere from the solar wind to the ionosphere down to the Earth's surface (Alfven & Falthammar 1963;Baker et al 1996;Barnes 1983;Nabert et al 2013). Knowledge of the wave properties and the current state of the sun can give us a clue to what is likely to be occurring at any particular latitude and local time (Ghamry et al 2016;Lin et al 1991;Nabert et al 2017).…”

Section: Observed Phenomena the Enhanced Occurrence Of Pulsationsmentioning

confidence: 99%

Geomagnetic Phenomena Observed by a Temporal Station at Ulu-Slim, Malaysia during The Storm of March 27, 2017

Arafa-Hamed¹,

Khalil²,

Nawawi³

et al. 2019

JSM

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A 3-axis fluxgate magnetometer was temporally setup for continuous recording during March 2017 at 3 о 54' 6" N, 101 о 29' 41" E, Ulu-Slim, Malaysia. On March 27th, a magnetic storm has been triggered by energetic solar wind emitted from a coronal hole on the sun that impacted the magnetosphere until the end of the measurement campaign on March 29th. The values measured at a sampling rate of 600 Hz are averaged to get a 1 Hz record from March 26 16:00 LT to March 29 12:00 LT. The 1 second data set is studied to deduce all magnetic phenomena captured during the magnetic storm. An overview of the complete record indicates the start of the storm and a complete absence of the typical diurnal variation of the total-field intensity on March 28. The diurnal variations are eliminated by subtracting a moving average of 100 samples from the recorded values. The residual shows a clear amplification of pulsations with the start of the storm. Pulsations enhancement are common around noon and is continuous on March 28th due to magnetotail activities during local night. Magnetospheric breathing as compression and expansion of the magnetosphere at long periods of 20 to 40 min is captured twice during the storm. An obvious occurrence of magnetotail reconnection is deduced by a sudden, steep increase of the total magnetic field with 50 nT at 01:30 LT on March 28. We conclude that the continuous recording of the magnetic field components provides very useful information about what processes are ongoing in space and how it might affect the logistics on the ground. The implementation of similar magnetometers as continuous observation stations would be of crucial benefits for Malaysia in both basic scientific and environmental aspects.

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A comprehensive analysis of the geomagnetic storms occurred during 18 February and 2 March 2014

Abstract: View related articles View Crossmark data Citing articles: 3 View citing articles A comprehensive analysis of the geomagnetic storms occurred during 18 February and

Cited by 16 publications

References 41 publications

Multiinstrument observations of a geomagnetic storm and its effects on the Arctic ionosphere: A case study of the 19 February 2014 storm

Multiinstrument observations of a geomagnetic storm and its effects on the Arctic ionosphere: A case study of the 19 February 2014 storm

Investigation of the relationship between the spatial gradient of total electron content (TEC) between two nearby stations and the occurrence of ionospheric irregularities

Geomagnetic Phenomena Observed by a Temporal Station at Ulu-Slim, Malaysia during The Storm of March 27, 2017

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