The interplanetary causes of geomagnetic activity during the 7–17 March 2012 interval: a CAWSES II overview

Journal of Space Weather and Space Climate

Martin Pätzold²  Janet U. Kozyra⁵  Walter D. Gonzalez⁶  Anthony J. Mannucci⁴  Olga P. Verkhoglyadova³  Kazunari Shibata¹  Ezequiel Echer⁶  Bruce T. Tsurutani⁴ 

[1] Kwasan Observatory, Kyoto University,607-8471,Japan;Department of Planetary Research, The Rhein Institute for the Environment, University of Cologne,50931Köln,Germany;Center for Space and Aeronomy Research, University of Alabama,Huntsville,AL35805,USA;Jet Propulsion Laboratory, California Institute of Technology,Pasadena,CA91109,USA;University of Michigan,Ann Arbor,MI48109-2143,USA;The Brazilian Institute for Space Research (INPE),Sao Jose dos Campos,SP12227-010,Brazil

关键词: solar wind;    ionosphere (equatorial);    shocks;    interplanetary coronal mass ejection;    storm;   

Others  :  800629
DOI  :  doi:10.1051/swsc/2013056

 received in 2013-07-20, accepted in 2013-12-11,  发布年份 2014

【 摘 要 】

This overview paper presents/discusses the major solar, interplanetary, magnetospheric, and ionospheric features of the CAWSES II interval of study: 7–17 March 2012. Magnetic storms occurred on 7, 9, 12, and 15 March with peak SYM-H intensities of −98 nT, −148 nT, −75 nT (pressure corrected), and −79 nT, respectively. These are called the S1, S2, S3, and S4 events. Although three of the storm main phases (S1, S3, and S4) were caused by IMF Bsouth sheath fields and the S2 event was associated with a magnetic cloud (MC), the detailed scenario for all four storms were different. Two interplanetary features with unusually high temperatures and intense and quiet magnetic fields were identified located antisunward of the MCs (S2 and S3). These features are signatures of either coronal loops or coronal sheaths. A high speed stream (HSS) followed the S4 event where the presumably southward IMF Bz components of the Alfvén waves extended the storm “recovery phase” by several days. The ICME-associated shocks were particularly intense. The fast forward shock for the S2 event had a magnetosonic Mach number of ~9.4, the largest in recorded history. All of the shocks associated with the ICMEs created sudden impulses (SI+s) at Earth. The shocks preceding the S2 and S3 magnetic storms caused unusually high SI+ intensities of ~60 and 68 nT, respectively. Many further studies on various facets of this active interval are suggested for CAWSES II researchers and other interested parties.

【 授权许可】

   
© B.T. Tsurutani et al., Published by EDP Sciences 2014

【 图 表 】

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