Explicit characteristics of evolutionary‐type plasma bubbles observed from Equatorial Atmosphere Radar during the low to moderate solar activity years 2010–2012

DOI Web Site Web Site 被引用文献13件 参考文献48件
  • K. K. Ajith
    Indian Institute of Geomagnetism Navi Mumbai India
  • S. Tulasi Ram
    Indian Institute of Geomagnetism Navi Mumbai India
  • M. Yamamoto
    Research Institute for Sustainable Humanosphere Kyoto University Uji Japan
  • T. Yokoyama
    National Institute of Information and Communications Technology Tokyo Japan
  • V. Sai Gowtam
    Indian Institute of Geomagnetism Navi Mumbai India
  • Y. Otsuka
    Solar Terrestrial Environment Laboratory Nagoya University Nagoya Japan
  • T. Tsugawa
    National Institute of Information and Communications Technology Tokyo Japan
  • K. Niranjan
    Department of Physics Andhra University Visakhapatnam India

書誌事項

公開日
2015-02
資源種別
journal article
権利情報
  • http://onlinelibrary.wiley.com/termsAndConditions#vor
DOI
  • 10.1002/2014ja020878
公開者
American Geophysical Union (AGU)

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説明

<jats:title>Abstract</jats:title><jats:p>Using the fan sector backscatter maps of 47 MHz Equatorial Atmosphere Radar (EAR) at Kototabang (0.2°S geographic latitude, 100.3°E geographic longitude, and 10.4°S geomagnetic latitude), Indonesia, the spatial and temporal evolution of equatorial plasma bubbles (EPBs) were examined to classify the evolutionary‐type EPBs from those which formed elsewhere and drifted into the field of view of radar. A total of 535 EPBs were observed during the low to moderate solar activity years 2010–2012, out of which about 210 (~39%) are of evolving type and the remaining 325 (~61%) are drifting‐in EPBs. In general, both the evolving‐type and drifting‐in EPBs exhibit predominance during the postsunset hours of equinoxes and December solstices. Interestingly, a large number of EPBs were found to develop even a few minutes prior to the apex sunset during equinoxes. Further, the occurrence of evolving‐type EPBs exhibits a clear secondary peak around midnight (2300–0100 LT), primarily, due to higher rate of occurrence during the postmidnight hours of June solstices. A significant number (~33%) of postmidnight EPBs generated during June solstices did not exhibited any clear zonal drift, while about 14% of EPBs drifted westward. Also, the westward drifting EPBs are confined only to June solstices. The responsible mechanisms for the genesis of fresh EPBs during postmidnight hours were discussed in light of equatorward meridional winds in the presence of weak westward electric fields.</jats:p>

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