Study of equatorial plasma bubbles using all sky imager and scintillation technique from Kolhapur station: a case study

Sharma, Ashok; Gurav, O.B.; Gaikwad, H.P.; Chavan, G.A.; Nade, D.P.; Nikte, S.S.; Ghodpage, R. N.; Patil, P. T.

doi:10.1007/s10509-018-3303-4

Cited by 12 publications

(4 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The different aspects of EPBs have been studied by many researchers such as occurrence characteristics (e.g., Candido et al, 2011;Makela et al, 2004;Sahai et al, 1994;Sharma et al, 2014;Sun et al, 2016), morphology and evolution (e.g., Aggson et al, 1996;Huba et al, 2015;Wu et al, 2017), statistical features of EPBs (e.g., Narayanan et al, 2017;Sinha & Raizada, 2000;Sun et al, 2016), and zonal drift velocity (e.g., Abalde et al, 2004;Immel et al, 2004;Mukherjee & Shetti, 2008;Nade et al, 2013;Paulino et al, 2011;Pimenta et al, 2001;Taori et al, 2013;Yao & Makela, 2007). However, there are different techniques to monitor and study the evolution and characteristics of these large-scale structures (EPBs) such as incoherent scatter radar (e.g., Fejer et al, 1991), VHF spaced receiver system (e.g., Bhattacharyya et al, 2003;Sharma et al, 2018), Fabry-Pérot interferometer (e.g., Sahai et al, 1992), GPS (e.g., Haase et al, 2011;Ji et al, 2011;Nade et al, 2015), and ASI (e.g., Fagundes et al, 1997;Ghodpage et al, 2018;Kishore & Mukherjee, 2007;Nade et al, 2013;Sobral et al, 2009;Taori & Sindhya, 2014). Sun et al (2016) investigated the statistical features of EPBs using airglow images from 2012 to 2014, which lies in the increasing phase of 24th solar cycle from a ground-based network of four ASIs in the equatorial region of China.…”

Section: Introductionmentioning

confidence: 99%

Zonal Drift Velocity of Equatorial Plasma Bubbles During Ascending Phase of 24th Solar Cycle Using All‐Sky Imager Over Kolhapur, India

et al. 2018

Self Cite

View full text Add to dashboard Cite

This paper reports the statistical analysis of zonal drift velocity of equatorial plasma bubbles (EPBs) inferred from advanced optical technique (all‐sky imager) with OI 630.0‐nm airglow emission from January to April of 2011 to 2013. Over 143 nights of observations have been carried out using all‐sky imager over low‐latitude station Kolhapur (16.8°N, 74.2°E; 10.6°N dip latitude), out of which 58 nights showed signatures of EPBs. We study the hourly, monthly, and seasonal variation in zonal drift velocity of EPBs. Also, the magnetically disturbed nights (Ap > 18) are separately studied. It is observed that (a) the daily peak zonal drift velocity is seen to be positively correlated to corresponding daily averaged 10.7‐cm solar flux. (b) The zonal drift velocity is found to be larger in the equinox months than that of winter months. (c) During the disturbed nights the zonal drift velocity gets slower and one of the disturbed nights showed the latitudinal variation in zonal drift velocity during the development phase of EPBs before midnight hours. We suggest that this variation might be occurred due to the disturbance dynamo electric fields at low latitude, which reduces the EPBs' eastward velocity. (d) The zonal drift velocity of EPBs presented in this paper is in good agreement with the previous studies as well as the HWM‐07 model values.

show abstract

Section: Introductionmentioning

confidence: 99%

Zonal Drift Velocity of Equatorial Plasma Bubbles During Ascending Phase of 24th Solar Cycle Using All‐Sky Imager Over Kolhapur, India

et al. 2018

Self Cite

View full text Add to dashboard Cite

show abstract

“…The raw images inferred from ASI are processed using the averaging method which includes several steps. More details about the ASI technique as well as the image processing method can be found in Sharma et al, [2017aSharma et al, [ , 2018. In addition to optical observations, we also used h'F (km)…”

Section: Methodsmentioning

confidence: 99%

Occurrence climatology of equatorial plasma bubbles (EPBs) using optical observations over Kolhapur, India during solar cycle-24

Gurav

Ghodpage

Patil

et al. 2020

Annals of Geophysics

View full text Add to dashboard Cite

In this paper, the occurrence characteristics of the equatorial plasma bubbles (EPBs) using OI 630.0 nm all sky imager (ASI) night airglow observations over Kolhapur (16.8o N, 74.2o E, 10.6o dip. Lat.) during the solar cycle-24 are presented. These results are discussed in terms of season, solar and magnetic activity during years 2011 to 2018. The ASI observations were only carried out during January to May and October to December months due to unfavorable weather conditions. The results suggest that while January, February and December are the only months where EPBs were found to occur over Kolhapur in any year, but the percentage of occurrence of EPBs during these months suggests their low occurrence rate during solar minimum. A total of 683 nights of observations were carried, out of which, 93 nights are found to be magnetically disturbed nights having Ap>18. In addition, the ASI observations are also correlated with Pre-Reversal Enhancement of the vertical drift of the evening sector at Tirunelveli on few storm events for comparison. The important findings of this study are: 1) increase in the occurrence of EPBs with respect to the solar activity; 2) suppression of EPBs on 71 disturbed nights, while enhancement of EPBs on 22 nights under magnetic disturbance; 3) EPBs occurrence during equinox months is found to be higher than winter months during ascending phase of solar cycle-24.; and, 4) EPBs are mostly observed in the pre-midnight sector in the high solar activity (HSA) period, while they are seen in the post-midnight to dawn sector during the low solar activity (LSA) period. We also noticed non-occurrence of EPBs during equinox month in the year 2018 which seems to be peculiar and needs further investigations.

show abstract

“…Spogli et al, 2016;Lühr et al, 2014;Bhattacharyya et al, 2003;Rao et al, 1997). Sharma et al (2018) suggested that small-scale structures may be abundantly available within the largely depleted EPBs, becoming the cause of L-band scintillation. Therefore, the results presented by Xiong et al (2016a) and Wan et al (2018) could be explained because deep EPBs involve steep density gradients and large background density which would create the small-scale irregularities.…”

Section: Local-time Distribution Of Ionospheric Irregularitiesmentioning

confidence: 99%

“…The effects of geomagnetic disturbances and changes in solar activity on ionospheric irregularity characteristics are of scientific interest and have been investigated in multiple studies (e.g. Palmroth et al, 2000;Sobral et al, 2002;Huang Figure 8. Scatter plots of the latitude distribution of ionospheric irregularities observed for the period from October 2014 to October 2018.…”

Section: Magnetic-and Solar-activity Dependence Of Ionospheric Irregumentioning

confidence: 99%

Traits of sub-kilometre F-region irregularities as seen with the Swarm satellites

2020

View full text Add to dashboard Cite

Abstract. During the night, in the F-region, equatorial ionospheric irregularities manifest as plasma depletions observed by satellites, and they may cause radio signals to fluctuate. In this study, the distribution characteristics of ionospheric F-region irregularities in the low latitudes were investigated using 16 Hz electron density observations made by a faceplate which is a component of the electric field instrument (EFI) onboard Swarm satellites of the European Space Agency (ESA). The study covers the period from October 2014 to October 2018 when the 16 Hz electron density data were available. For comparison, both the absolute (dNe) and relative (dNe∕Ne) density perturbations were used to quantify the level of ionospheric irregularities. The two methods generally reproduced the local-time (LT), seasonal and longitudinal distribution of equatorial ionospheric irregularities as shown in earlier studies, demonstrating the ability of Swarm 16 Hz electron density data. A difference between the two methods was observed based on the latitudinal distribution of ionospheric irregularities where (dNe) showed a symmetrical distribution about the magnetic equator, while dNe∕Ne showed a magnetic-equator-centred Gaussian distribution. High values of dNe and dNe∕Ne were observed in spatial bins with steep gradients of electron density from a longitudinal and seasonal perspective. The response of ionospheric irregularities to geomagnetic and solar activities was also investigated using Kp index and solar radio flux index (F10.7), respectively. The reliance of dNe∕Ne on solar and magnetic activity showed little distinction in the correlation between equatorial and off-equatorial latitudes, whereas dNe showed significant differences. With regard to seasonal and longitudinal distribution, high dNe and dNe∕Ne values were often found during quiet magnetic periods compared to magnetically disturbed periods. The dNe increased approximately linearly from low to moderate solar activity. Using the high-resolution faceplate data, we were able to identify ionospheric irregularities on the scale of only a few hundred of metres.

show abstract

Study of equatorial plasma bubbles using all sky imager and scintillation technique from Kolhapur station: a case study

Cited by 12 publications

References 29 publications

Zonal Drift Velocity of Equatorial Plasma Bubbles During Ascending Phase of 24th Solar Cycle Using All‐Sky Imager Over Kolhapur, India

Zonal Drift Velocity of Equatorial Plasma Bubbles During Ascending Phase of 24th Solar Cycle Using All‐Sky Imager Over Kolhapur, India

Occurrence climatology of equatorial plasma bubbles (EPBs) using optical observations over Kolhapur, India during solar cycle-24

Traits of sub-kilometre F-region irregularities as seen with the Swarm satellites

Contact Info

Product

Resources

About