Low‐latitude Pi2 pulsations during intervals of quiet geomagnetic conditions (<b><i>K</i><sub><i>p</i></sub>≤1</b>)

DOI Web Site Web Site 被引用文献3件 オープンアクセス
  • H.‐J. Kwon
    School of Space Research Kyung Hee University Yongin South Korea
  • K.‐H. Kim
    School of Space Research Kyung Hee University Yongin South Korea
  • C.‐W. Jun
    Solar‐Terrestrial Environment Laboratory Nagoya University Nagoya Japan
  • K. Takahashi
    Applied Physics Laboratory Johns Hopkins University Laurel Maryland USA
  • D.‐H. Lee
    School of Space Research Kyung Hee University Yongin South Korea
  • E. Lee
    School of Space Research Kyung Hee University Yongin South Korea
  • H. Jin
    School of Space Research Kyung Hee University Yongin South Korea
  • J. Seon
    School of Space Research Kyung Hee University Yongin South Korea
  • Y.‐D. Park
    Solar and Space Weather Research Group Korea Astronomy and Space Science Institute Daejeon South Korea
  • J. Hwang
    Solar and Space Weather Research Group Korea Astronomy and Space Science Institute Daejeon South Korea

書誌事項

公開日
2013-10
権利情報
  • http://onlinelibrary.wiley.com/termsAndConditions#vor
DOI
  • 10.1002/jgra.50582
公開者
American Geophysical Union (AGU)

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説明

<jats:p>It has been reported that Pi2 pulsations can be excited under extremely quiet geomagnetic conditions (<jats:italic>K</jats:italic><jats:sub><jats:italic>p</jats:italic></jats:sub>=0). However, there have been few comprehensive reports of Pi2 pulsations in such a near ground state magnetosphere. To understand the characteristics of quiet‐time Pi2 pulsations, we statistically examined Pi2 events observed on the nightside between 1800 and 0600 local time at the low‐latitude Bohyun (BOH, <jats:italic>L</jats:italic> = 1.35) station in South Korea. We chose year 2008 for analysis because geomagnetic activity was unusually low in that year. A total of 982 Pi2 events were identified when <jats:italic>K</jats:italic><jats:sub><jats:italic>p</jats:italic></jats:sub>≤1. About 80% of the Pi2 pulsations had a period between 110 and 300 s, which significantly differs from the conventional Pi2 period from 40 to 150 s. Comparing Pi2 periods and solar wind conditions, we found that Pi2 periods decrease with increasing solar wind speed, consistent with the result of Troitskaya (1967). The observed wave properties are discussed in terms of plasmaspheric resonance, which has been proposed for Pi2 pulsations in the inner magnetosphere. We also found that Pi2 pulsations occur quasi‐periodically with a repetition period of ∼23–38 min. We will discuss what determines such a recurrence time of Pi2 pulsations under quiet geomagnetic conditions.</jats:p>

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