Plasma bubble monitoring by TEC map and 630nm airglow image

Takahashi, H.; Wrasse, C. M.; Otsuka, Yuichi; Ivo, A.; Gomes, Vitor Conrado Faria; Paulino, Igo; Medeiros, A. F.; Denardini, Clezio Marcos; Sant’Anna, N.; Shiokawa, K.

doi:10.1016/j.jastp.2015.06.003

Cited by 46 publications

(59 citation statements)

References 24 publications

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“…If no data are found in the area, the running average area expands to 5 × 5 elements (∼ 250 km × 250 km). If the problem persists, the area expands up to 21×21 elements (∼ 1000 km × 1000 km) (Takahashi et al, , 2015. In general, the spatial resolution is 50 to 100 km in the southeastern part of Brazil and 200 to 300 km in the northeastern part .…”

Section: Observationsmentioning

confidence: 99%

“…Characteristics of EPBs have been extensively studied using different techniques such as VHF radars (Tsunoda, 1981;Abdu et al, 2009), rockets Muralikrishna et al, 2007), ionosondes (Abdu et al, 1983(Abdu et al, , 2003(Abdu et al, , 2012, optical imagers (Pimenta et al, 2003;Arruda et al, 2006;Paulino et al, 2011), GNSS receivers (De Rezende et al, 2007;Takahashi et al, 2014Takahashi et al, , 2015, and satellites (Huang et al, 2002(Huang et al, , 2013McNamara et al, 2013;Park et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

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Characteristics of equatorial plasma bubbles observed by TEC map based on ground-based GNSS receivers over South America

et al. 2018

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Abstract. A ground-based network of GNSS receivers has been used to monitor equatorial plasma bubbles (EPBs) by mapping the total electron content (TEC map). The large coverage of the TEC map allowed us to monitor several EPBs simultaneously and get characteristics of the dynamics, extension and longitudinal distributions of the EPBs from the onset time until their disappearance. These characteristics were obtained by using TEC map analysis and the keogram technique. TEC map databases analyzed were for the period between November 2012 and January 2016. The zonal drift velocities of the EPBs showed a clear latitudinal gradient varying from 123 m s −1 at the Equator to 65 m s −1 for 35• S latitude. Consequently, observed EPBs are inclined against the geomagnetic field lines. Both zonal drift velocity and the inclination of the EPBs were compared to the thermospheric neutral wind, which showed good agreement. Moreover, the large two-dimensional coverage of TEC maps allowed us to study periodic EPBs with a wide longitudinal distance. The averaged values observed for the inter-bubble distances also presented a clear latitudinal gradient varying from 920 km at the Equator to 640 km at 30 • S. The latitudinal gradient in the inter-bubble distances seems to be related to the difference in the zonal drift velocity of the EPB from the Equator to middle latitudes and to the difference in the westward movement of the terminator. On several occasions, the distances reached more than 2000 km. Inter-bubble distances greater than 1000 km have not been reported in the literature.

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Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Characteristics of equatorial plasma bubbles observed by TEC map based on ground-based GNSS receivers over South America

et al. 2018

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“…During quiet times, the prereversal enhancement (PRE) of the zonal electric field is responsible for the enhanced upward E × B drift after sunset, which elevates the ionospheric height and subsequently amplifies the growth rate of R-T The morphological features and spatial/temporal variability of EPBs have been widely investigated via case studies and statistical analysis using different observational methods. Moreover, with the fast-growing and global availability of ground-based Global Navigation Satellite Systems (GNSS) measurements and space-based radio occultation data, the evolution characteristics of EPBs can be monitored continuously on both global or regional scales (Aa et al, 2018;Barros et al, 2018;Buhari et al, 2014Buhari et al, , 2017Cherniak et al, 2014;Katamzi-Joseph et al, 2017;Ma & Maruyama, 2006;Nishioka et al, 2008;Takahashi et al, 2015). The spatial variation of EPBs can be derived from the dark streaks of emission depletion in optical observations from ground-based all-sky imagers (ASIs) or space-based ultraviolet (UV) imaging spectrographs (Comberiate & Paxton, 2010;Hickey et al, 2018;Kelley et al, 2003;Kil et al, 2009;Makela, 2006;Martinis et al, 2015;Otsuka et al, 2002;Shiokawa et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

Coordinated Ground‐Based and Space‐Based Observations of Equatorial Plasma Bubbles

Zou

Eastes

et al. 2020

JGR Space Physics

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This paper presents coordinated and fortuitous ground-based and spaceborne observations of equatorial plasma bubbles (EPBs) over the South American area on 24 October 2018, combining the following measurements: Global-scale Observations of Limb and Disk far ultraviolet emission images, Global Navigation Satellite System total electron content data, Swarm in situ plasma density observations, ionosonde virtual height and drift data, and cloud brightness temperature data. The new observations from the Global-scale Observations of Limb and Disk/ultraviolet imaging spectrograph taken at geostationary orbit provide a unique opportunity to image the evolution of plasma bubbles near the F peak height over a large geographic area from a fixed longitude location. The combined multi-instrument measurements provide a more integrated and comprehensive way to study the morphological structure, development, and seeding mechanism of EPBs. The main results of this study are as follows: (1) The bubbles developed a westward tilted structure with 10-15 • inclination relative to the local geomagnetic field lines, with eastward drift velocity of 80-120 m/s near the magnetic equator that gradually decreased with increasing altitude/latitude. (2) Wave-like oscillations in the bottomside F layer and detrended total electron content were observed, which are probably due to upward propagating atmospheric gravity waves. The wavelength based on the medium-scale traveling ionospheric disturbance signature was consistent with the interbubble distance of ∼500-800 km. (3) The atmospheric gravity waves that originated from tropospheric convective zone are likely to play an important role in seeding the development of this equatorial EPBs event.Plain Language Summary This study presents multi-instrument observations of equatorial plasma density depletions occurred on 24 October 2018 by using Global-scale Observations of Limb and Disk far ultraviolet images, Global Navigation Satellite System total electron content data, electron density measurements from Swarm satellite, ionosonde measurements, and cloud temperature data. This multi-instrument study generated an integrated and detailed image revealing both large-scale and mesoscale structures of the equatorial plasma depletion. Our results also suggest that atmospheric gravity waves originating from tropospheric convection activity could play a significant seeding role in the development of equatorial plasma bubbles. Key Points: • Combined GOLD/UV spectrograph images and ground-based TEC data revealed EPB features and development over a large geographic area • Bottomside F layer oscillations and traveling ionospheric disturbance were observed by ionosonde and detrended TEC results • Atmospheric gravity waves likely play an important role in seeding the R-T instability and the development of this EPB event Correspondence to: E. Aa,

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“…Looking the gradient in terms of the total electron content (TEC unit of 1 × 10 16 /m 2 col), it varies from a few total electron content unit, 1 TECU = 10 16 el m −2 (TECU) along the magnetic equator region to 20–50 TECU at the crest region depending on the day and season [ Bagiya et al ., ]. In the case of plasma bubbles, the TEC gradient is much steep, a difference of 30–50 TECU from the inside to outside of the bubble with a distance of hundreds of kilometers [ Takahashi et al ., ]. In addition to the spatial gradient of TEC, radio wave propagation inside of the plasma bubbles is affected by spatial irregularity of plasma density causing radio wave scintillations [ Kintner et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Ionospheric TEC Weather Map Over South America

et al. 2016

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Ionospheric weather maps using the total electron content (TEC) monitored by ground‐based Global Navigation Satellite Systems (GNSS) receivers over South American continent, TECMAP, have been operationally produced by Instituto Nacional de Pesquisas Espaciais's Space Weather Study and Monitoring Program (Estudo e Monitoramento Brasileiro de Clima Especial) since 2013. In order to cover the whole continent, four GNSS receiver networks, (Rede Brasileiro de Monitoramento Contínuo) RBMC/Brazilian Institute for Geography and Statistics, Low‐latitude Ionospheric Sensor Network, International GNSS Service, and Red Argentina de Monitoreo Satelital Continuo, in total ~140 sites, have been used. TECMAPs with a time resolution of 10 min are produced in 12 h time delay. Spatial resolution of the map is rather low, varying between 50 and 500 km depending on the density of the observation points. Large day‐to‐day variabilities of the equatorial ionization anomaly have been observed. Spatial gradient of TEC from the anomaly trough (total electron content unit, 1 TECU = 1016 el m−2 (TECU) <10) to the crest region (TECU > 80) causes a large ionospheric range delay in the GNSS positioning system. Ionospheric plasma bubbles, their seeding and development, could be monitored. This plasma density (spatial and temporal) variability causes not only the GNSS‐based positioning error but also radio wave scintillations. Monitoring of these phenomena by TEC mapping becomes an important issue for space weather concern for high‐technology positioning system and telecommunication.

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Plasma bubble monitoring by TEC map and 630nm airglow image

Cited by 46 publications

References 24 publications

Characteristics of equatorial plasma bubbles observed by TEC map based on ground-based GNSS receivers over South America

Characteristics of equatorial plasma bubbles observed by TEC map based on ground-based GNSS receivers over South America

Coordinated Ground‐Based and Space‐Based Observations of Equatorial Plasma Bubbles

Ionospheric TEC Weather Map Over South America

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