日本地球惑星科学連合2019年大会

講演情報

[E] ポスター発表

セッション記号 P (宇宙惑星科学) » P-EM 太陽地球系科学・宇宙電磁気学・宇宙環境

[P-EM11] Dynamics of Magnetosphere and Ionosphere

2019年5月29日(水) 17:15 〜 18:30 ポスター会場 (幕張メッセ国際展示場 8ホール)

コンビーナ:中溝 葵(情報通信研究機構 電磁波研究所)、尾崎 光紀(金沢大学理工研究域電子情報学系)、藤本 晶子(九州工業大学)、堀 智昭(名古屋大学宇宙地球環境研究所)

[PEM11-P15] Spatial characteristics of the internal modulation of pulsating aurora: multi-point high-speed optical observations in Scandinavia

*川村 勇貴1細川 敬祐1大山 伸一郎2,3三好 由純2小川 泰信3栗田 怜2江袋 叡1藤井 良一4 (1.電気通信大学大学院 情報理工学研究科、2.名古屋大学宇宙地球環境研究所、3.国立極地研究所、4.情報・システム研究機構)

キーワード:脈動オーロラ、内部変調

Pulsating aurora (PsA) is a kind of diffuse aurora which almost always appears in the morning side during the recovery phase of auroral substorm. PsA typically has two characteristic temporal variations. One is so-called main pulsation whose period ranges from a few to a few tens of seconds. The other is a few Hz brightness modulation (internal modulation) which is often seen during the ON time of the main pulsation. Previous studies have suggested that the temporal variation of PsA is characterized by wave-particle interaction between whistler-mode chorus waves and high energy electrons in the magnetosphere. Especially, it has been indicated that there is one to one correspondence between the amplitude variation of chorus waves and the luminosity modulation of PsA.
Recent studies revealed the occurrence distribution of the frequency of the internal modulation. However, there have been no studies which analyzed the spatial distribution of the internal modulation.

To reveal the spatial characteristics of the internal modulation, we need to perform a frequency analysis of the internal modulation by using data from high speed optical instruments having wide spatial coverage. For this purpose, we make use of highly sensitive EMCCD cameras which have been operated in Sodankylä and Kevo in Finland, Tromsø in Norway, and Tjautjas in Sweden. In these observations, all-sky images are taken with a sampling rate of 100 Hz, which is sufficient to identify temporal variations of the internal modulation.

In the frequency analysis, we have employed all-sky images taken on March 15, 2018 (00:00 – 01:30 UT) in Sodankylä, Kevo, Tromsø, and Tjautjas. We computed the average frequency of the internal modulation from each pixel of the EMCCD cameras and derived the spatial distribution of their dominant frequencies. Regardless of the latitude, each pulsating patch was fluctuating at a similar frequency. We also derived the frequency spectrum of several pulsating patches existing at different positions in the north-south direction and found that those frequency spectrums of pulsating patches have peaks at about 3 Hz. These results indicate that the frequency of the internal modulation does not depend on the magnetic latitude, and the frequency of the internal modulation is collimated on 3 Hz.
In the presentation, we discuss why the frequency of the internal modulation concentrate on 3 Hz by taking into account the time of flight of PsA electrons.