JpGU-AGU Joint Meeting 2017

講演情報

[EE] 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-EM14] [EE] Dynamics in magnetosphere and ionosphere

2017年5月20日(土) 10:45 〜 12:15 ポスター会場 (国際展示場 7ホール)

コンビーナ:堀 智昭(東京大学大学院理学系研究科)、田中 良昌(国立極地研究所)、中溝 葵(情報通信研究機構 電磁波計測研究所)、尾崎 光紀(金沢大学理工研究域電子情報学系)

[PEM14-P05] A statistical study of the near-Earth magnetotail evolution duing substorms and pseudosubstorms with themis data

*福井 健人1町田 忍1宮下 幸長1家田 章正1三好 由純1Angelopoulos Vassilis2 (1.名古屋大学宇宙地球環境研究所、2.カリフォルニア大学ロサンゼルス校)

キーワード:substorm

Substorms and pseudosubstorms (pseudobreakups) are very similar phenomena. In terms of auroral morphology, pseudosubstorms are generally more localized and more short-lived, compared with substorms, and are not accompanied by poleward expansion. We examined auroral development for events from November 2007 through April 2010, using data from THEMIS all-sky imagers. We defined events accompanied and not accompanied by poleward expansion as substorms and pseudosubstorms, respectively. To understand the cause of auroral development, we investigated temporal and spatial development of the near-Earth magnetotail during substorms and pseudosubstorms, based on superposed epoch analysis of THEMIS data. We find that Vx begins to increase at -9.5 >X(GSM)>-11.5 Re around onset for both substorms and pseudosubstorms. This seems to be due to earthward flows caused by magnetic reconnection. Bz also increase around onset at -9.5 >X>-11.5 Re both substorms and pseudosubstorms. The amount and rate of Bz change are larger for substorms than for pseudosubstorms. In the earthward (-7.5 >X>-9.5 Re) and tailward (-11.5 >X>-15.5 Re) regions, Bz increases substantially for substorms, whereas it does not increase very much for pseudosubstorms. These results indicate that dipolarization is weaker for pseudosubstorms than for substorms, and the dipolarization region does not spread extensively for pseudosubstorms. In addition, Brms begins to increase at -6.5>X>-11.5 Re around onset both substorms and pseudosubstorms. The amount of Brms change is larger for substorms than for pseudosubstorms, indicating that waves are strongly induced for substorms. These waves are considered to be caused by instability, and the instability takes place in more for substorms and not in pseudosubstorms. We, therefore, suggest that the occurrence of the instability develops tailward to form the current disruption region and causes auroral poleward expansion. Meanwhile, the plasma and magnetic pressures increase at -6.5 >X>-7.5 Re after onset in association with dipolarization, particularly for substorms. The total pressure (the sum of the plasma and magnetic pressures) prior to the onset is larger in that region for substorms than for pseudosubstorms. At -7.5 >X>-9.5 Re the total pressure hardly differ between substorms and pseudosubstorms. Thus we conclude that the spatial gradient of the total pressure is a key that determines whether the current disruption take place, that is, whether initial activation develops into a substorm or into a subsiding pseudosubstorm.