Hemispheric asymmetries in the ionosphere response observed during the high-speed solar wind streams of the 24–28 August 2010

Zaourar, Naïma; Amory‐Mazaudier, Christine; Fleury, Rolland

doi:10.1016/j.asr.2017.01.048

Cited by 21 publications

(24 citation statements)

References 54 publications

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“…It showed that the geomagnetic fields at high latitudes oscillated drastically during the storm due to the influence of high-speed solar winds. This is in good consistency with previous discoveries of magnetic responses to high-speed solar winds at high latitudes regions [1,39], leading to ionosphere TEC variations. The asymmetry feature was also found between the northern hemisphere and southern hemisphere.…”

Section: Global Morphology Of Geomagnetic Stormssupporting

confidence: 92%

“…where S R (H) denotes the solar daily variation of the earth's magnetic field related to the regular ionospheric dynamo. λ denotes the magnetic dip angle of the given location, D iono represents the magnetic disturbance due to the disturbed ionosphere electric currents, H SYM represents SYM-H, the contributions of the electric currents in the magnetosphere (refer to Reference [1]).…”

Section: Calculation Of Geomagnetic Perturbationsmentioning

confidence: 99%

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Studying Ionosphere Responses to a Geomagnetic Storm in June 2015 with Multi-Constellation Observations

Liu

Wang

et al. 2018

Remote Sensing

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The Global Navigation Satellite System (GNSS) observations with global coverage and high temporal and spatial resolution, provide abundant and high-quality Earth-ionosphere observations. By calculating the total electron content (TEC), estimations from GNSS observables global and regional ionosphere TEC morphology can be further investigated. For the multiple constellation case, the numbers of ionosphere pierce points (IPP) has increased tremendously, and it is worth studying the features of the GNSS derived TEC under geomagnetic storms to show the benefits of multiple constellation measurements. With the Multi-GNSS Experiment (MGEX) observation data, ionosphere TEC responses to the geomagnetic storm on the 22 June 2015 were well studied. TEC perturbations were discovered, accompanied by ionosphere irregularities concentrating in high and middle latitudes. Through analysis of multi-GNSS observations, the Rate of TEC Index (ROTI) perturbations were proved to be generated by the geomagnetic storm, with simultaneous behaviors at different local times around the world, also indicating ionosphere scintillation. The ionosphere spatial gradient was also discussed with two short baseline MGEX sites; the maximum ionosphere gradient of 247.2 mm/km was found, due to ionosphere irregularity produced by the storm. This research has discussed ionosphere responses to geomagnetic storms with multi-GNSS data provided and has analyzed the availability of multi-GNSS observations to investigate ionosphere irregularity climatology. The proposed work is valuable for further investigation of GNSS performances under geomagnetic storms.

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Section: Global Morphology Of Geomagnetic Stormssupporting

confidence: 92%

Section: Calculation Of Geomagnetic Perturbationsmentioning

confidence: 99%

Studying Ionosphere Responses to a Geomagnetic Storm in June 2015 with Multi-Constellation Observations

Liu

Wang

et al. 2018

Remote Sensing

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“… D iono can be estimated using the following expression (Le Huy & Amory‐Mazaudier, ; Zaourar et al, ):

D_{iono} = normalΔ H - SYM - H \cdot cos ϕ - italicSq

where ΔH is the variation of H component obtained using , SYM − H is the estimation of the ring current and ϕ is the geomagnetic latitude. It is worth noting that D iono can be used to estimate ionospheric electric currents only on the dayside where they circulate.…”

Section: Data Set and Data Processingmentioning

confidence: 99%

Multivariable Comprehensive Analysis of Two Great Geomagnetic Storms of 2015

et al. 2018

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During the year 2015 two great geomagnetic storms (Dst < À200 nT) occurred on 17 March and 22 June. These two geomagnetic storms have similarities. They occurred during the same decreasing phase of the sunspot cycle 24. The interplanetary and magnetospheric environments were calm before the beginning of the storms. Both events were due to Coronal Mass Ejections and High-Speed Solar Wind. Variations of the solar wind velocity and the Bz component of the interplanetary magnetic field were also similar. Two key features that are different for these storms are UT time of the beginning (04:45 UT for 17 March and 18:33 UT for 22 June) and season (equinox and solstice). The comparison of the impact of the storms on the Earth ionosphere and magnetosphere has been performed using diverse parameters including global ionospheric maps of vertical total electron content, data from individual Global Navigation Satellite System receivers, ionosondes, magnetometers, and instruments from different space missions. Visualizing global ionospheric map data as the difference of vertical total electron content between consecutive days allowed understanding better the effect of the storms as a function of time of the beginning of the storm and of the season. It is shown that the presence or absence of scintillations in Global Navigation Satellite System signals during these two storms in African longitude sector is clearly related to the local time at a given station at the beginning of the storm.In addition to many data sets scientists also have access to modeling results that allow them interpreting their observations. Theoretical work carried out by Fuller-Rowell et al. (1994) defined the response of the thermosphere during a magnetic storm due to thermal expansion of the atmosphere with transport of KASHCHEYEV ET AL. 5000

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“…In equation (3), STEC is in TECU with 1 TECU = 10 16 electrons/m 3 , t k À t k À 1 is the time difference between successive epoch = 30 s. ROT is converted in TECU/min by multiplying by 60 s (Azzouzi et al, 2015;Zaourar et al, 2017).…”

Section: Space Weathermentioning

confidence: 99%

The Response of African Equatorial/Low‐Latitude Ionosphere to 2015 St. Patrick's Day Geomagnetic Storm

2018

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Total electron content (TEC) has been used to study the response of the African equatorial/low‐latitude ionosphere to the 17 March 2015 intense storm. Daily variations of symmetric H index, z component of interplanetary magnetic field, polar cap index, and H component of the Earth's magnetic field were analyzed along with TEC obtained from stations classified into western (11.53°E to 5.24°W) and eastern (25.00°E to 40.20°E) sectors. Storm time behavior of TEC was compared with the mean TEC of quiet days. TEC was enhanced over both sectors at the beginning of the storm while it reduced after the main phase as a result of prompt penetration of electric field and disturbance dynamo electric field (DDEF), respectively. The magnetic effect of the disturbed ionospheric electric current showed oscillations and minima in response to prompt penetration of electric field, which further enhanced the equatorial ionization anomaly. The effect of DDEF estimated from the ionospheric disturbance dynamo manifested in the form of decrease in the amplitude of the horizontal component of the Earth magnetic field (H) several hours after the beginning of the disturbance and during the recovery phase. Consequently, ionospheric irregularities were suppressed over all stations in both sectors on 17 and 18 March due to westward DDEF. On the 19 March, however, there was a difference in the pattern of irregularities over both sectors.

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Hemispheric asymmetries in the ionosphere response observed during the high-speed solar wind streams of the 24–28 August 2010

Cited by 21 publications

References 54 publications

Studying Ionosphere Responses to a Geomagnetic Storm in June 2015 with Multi-Constellation Observations

Studying Ionosphere Responses to a Geomagnetic Storm in June 2015 with Multi-Constellation Observations

Multivariable Comprehensive Analysis of Two Great Geomagnetic Storms of 2015

The Response of African Equatorial/Low‐Latitude Ionosphere to 2015 St. Patrick's Day Geomagnetic Storm

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