Multi-instrument observations of plasma features in the Arctic ionosphere during the main phase of a geomagnetic storm in December 2006

Wu, Yewen; Liu, Ruiyuan; Zhang, Beichen; Wu, Zhensen; Hu, Hongqiao; Zhang, Shun-rong; Zhang, Qinghe; Liu, Junming; Honary, F.

doi:10.1016/j.jastp.2013.07.004

Cited by 9 publications

(9 citation statements)

References 28 publications

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“…A is Ne at h 0 , which is the top height of an observational electron density profile. The c is a parameter for fitting the topside ionospheric Ne (Wu, Liu, Zhang, Wu, Hu, et al, ; Wu, Liu, Zhang, Wu, Xu, et al, ).…”

Section: Methodsmentioning

confidence: 99%

“…There are about 400,000 Ne profiles left in the polar region after a process of elimination for data quality (Wu, Liu, Zhang, Wu, Hu, et al, ). The criteria are as follows: There should be enough observations above the maximum Ne value in one profile, that is, Ne at the height h 0 is less than one fifth of the maximum Ne. The maximum Ne should be less than 1.1 * 10 7 electrons per cubic centimeter. The height of maximum Ne should be larger than 90 km. …”

Section: Datamentioning

confidence: 99%

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The UT Variation of the Polar Ionosphere Based on COSMIC Observations

Liu

Zhang

et al. 2019

JGR Space Physics

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Mean polar electron content (mPEC) is used to analyze the polar ionosphere in both the Antarctic and Arctic. The mPEC is calculated over the polar region covering geographic latitudes higher than 60°from the global distributed vertical total electron contents based on electron density profiles observed by Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC). Using this parameter, the universal time (UT) variation of the polar ionosphere is quantitatively characterized. This UT variation exists an opposite phase (i.e., a 12-hr phase difference) between them. The mPEC standard deviation (SD) in the Antarctic is larger in summer and autumn (being 1.37 and 0.78 TECu, respectively) and smaller in winter (0.29 TECu) and spring (0.61 TECu). The SD in the Arctic, however, is the largest in winter (0.14 TECu). In other seasons, the SD is less than 0.1 TECu. (being 0.07 TECu in spring, 0.05 TECu in summer, and 0.08 TECu in autumn, respectively). We use SD over the mean value to describe relative intensity of mPEC variations. This relative intensity is larger in winter for both Antarctic and Arctic regions. The UT variation in intensity is much stronger in the Antarctic than in the Arctic. These characteristics are attributed to the fact that the separation of the geomagnetic pole and geographic pole is dihedral and the angle is larger in the Antarctic. The larger angle causes more electrons transported into the polar region when the geomagnetic pole is on the dayside and fewer electrons transported into the polar region when the geomagnetic pole is on the nightside. With the development of the radio occultation (RO) measurements, large amount of ionospheric data have been collected globally (Fong et al., 2007; Lei et al., 2007; Liou et al., 2005; Yue et al., 2013), making it

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Section: Methodsmentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

The UT Variation of the Polar Ionosphere Based on COSMIC Observations

Liu

Zhang

et al. 2019

JGR Space Physics

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“…On the other hand, Lei et al [] and Wang et al [] have examined such mechanisms as dynamics of neutral winds and changing O/N 2 composition using TIEGCM simulations and have come to the opposite conclusion that the penetration electric field mechanism should play the main role for the positive storm effect, while the neutral winds and chemical composition play a secondary role. Indeed, at that time, the high‐latitude ionosphere got a relatively small energy input from the auroral precipitations, and hence, the thermosphere had no time to be strongly disturbed, at least in comparison with thermosphere heating at the main phase according to the studies by Wei et al [] and Wu et al []. Moreover, direct observations, reported by Wu et al [] demonstrated convincingly that at high latitude the neutral wind effect was weak during that time.…”

Section: Discussionmentioning

confidence: 84%

“…Ionospheric effects during the 14–16 December 2006 storm were considered in numerous studies [ Lei et al , ; Pedatella et al , ; Wang et al , ; de Jesus et al , ; Kikuchi et al , ; Leonovich et al , ; Wei et al , ; Klimenko and Klimenko , ; Suvorova et al , , , ; Wu et al , ]. In particular, Suvorova et al [] emphasized that the positive ionospheric storm was unusually long and was accompanied by several FEE enhancements that occurred from the initial to late recovery phases.…”

Section: Introductionmentioning

confidence: 99%

Effects of ionizing energetic electrons and plasma transport in the ionosphere during the initial phase of the December 2006 magnetic storm

et al. 2016

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The initial phase of a major geomagnetic storm on 14 December 2006 was selected in order to investigate the ionizing effect of energetic electrons in the ionosphere. The global network of GPS receivers was used to analyze the total electron content (TEC). A strong positive ionospheric storm of ~20 TEC units (TECU) with ~6 h duration was observed on the dayside during the interval of northward interplanetary magnetic field. At the same time, the NOAA/POES satellites observed long‐lasting intense fluxes of >30 keV electrons in the topside ionosphere at middle and low latitudes, including a near‐equatorial forbidden zone outside of the South Atlantic Anomaly (SAA). We found that the TEC increases overlapped well with the enhancements of energetic electrons. Modeling of the ionospheric response by using a Global Self‐consistent Model of the Thermosphere, Ionosphere, and Protonosphere, based on the standard mechanisms of plasma transport, could only partially explain the ionospheric response and was unable to predict the long‐duration increase of TEC. For the energetic electrons, we estimated the ionizing effect of ~45 TECU and ~23 TECU in the topside ionosphere, respectively, inside and outside of SAA. The ionizing effect contributed from 50% to 100% of TEC increases and provided the long duration and wide latitudinal extension of the positive ionospheric storm. This finding is a very important argument in supporting significant ionizing effect of energetic electrons in the storm time ionosphere both at middle and low latitudes.

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“…It is better to look into ionospheric parameter obtained by other facilities available. The Global Positioning System (GPS) can suffer from short‐term signal fading and rapid phase changes during ionospheric disturbances [e.g., Mitchell et al ., ; Wu et al ., ]. A specially modified GPS receiver system for recording the phase and amplitude of the L1 signals and calculating the scintillation index and TEC is called GISTM (GPS Ionospheric Scintillation and TEC Monitor).…”

Section: Statistical Studymentioning

confidence: 99%

F‐lacuna at cusp latitude and its associated TEC variation

et al. 2014

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As a frequent phenomenon occurring during summer days in high-latitude ionosphere, the F-lacuna manifests itself as disappearance of F region ionogram traces. Based on the 7.5 min interval Digisonde ionograms recorded at Zhongshan station (69.4°S, 76.4°E geographic coordinates; 74.5°S, 96.0°E corrected geomagnetic coordinates), we present temporal characteristics of the F-lacuna, as well as its correlation with geomagnetic activity, interplanetary magnetic field, and colocated TEC. Magnetic Local Time (MLT) distribution of the F-lacuna occurrence exhibits a dawn-dusk asymmetry. All types of F-lacuna favor the dawn sector, mainly occurring at 08:00-11:00MLT for F1 and total lacuna, 6:00-8:00MLT for F2-lacuna. The magnetic activity is found to have a strong positive correlation with the F2 and total lacuna. F2-lacuna occurrence is favored by southward component of interplanetary magnetic field (IMF), and total lacuna by high values of either eastward or westward component. It is worth to mention that the F-lacuna associates with the simultaneous total electron content (TEC) condition which has a positive correlation with F1-lacuna occurrence, while a strong negative correlation with the F2 and total lacuna. The associated TEC variation may provide a significant evidence for interpreting the F-lacuna phenomenon.

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Multi-instrument observations of plasma features in the Arctic ionosphere during the main phase of a geomagnetic storm in December 2006

Cited by 9 publications

References 28 publications

The UT Variation of the Polar Ionosphere Based on COSMIC Observations

The UT Variation of the Polar Ionosphere Based on COSMIC Observations

Effects of ionizing energetic electrons and plasma transport in the ionosphere during the initial phase of the December 2006 magnetic storm

F‐lacuna at cusp latitude and its associated TEC variation

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