Comparison of Magnetospheric Multiscale ion jet signatures with predicted reconnection site locations at the magnetopause

被引:21
|
作者
Petrinec, S. M. [1 ]
Burch, J. L. [2 ]
Fuselier, S. A. [2 ,3 ]
Gomez, R. G. [2 ]
Lewis, W. [2 ]
Trattner, K. J. [4 ]
Ergun, R. [4 ]
Mauk, B. [5 ]
Pollock, C. J. [6 ]
Schiff, C. [6 ]
Strangeway, R. J. [7 ]
Russell, C. T. [7 ]
Phan, T. -D. [8 ]
Young, D. [2 ]
机构
[1] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA
[2] Southwest Res Inst, San Antonio, TX USA
[3] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA
[4] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA
[5] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA
[6] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA
[7] Univ Calif Los Angeles, Los Angeles, CA USA
[8] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA
基金
美国国家科学基金会;
关键词
MAGNETIC-FIELD; DAYSIDE MAGNETOPAUSE; NORTHWARD IMF; EARTHS MAGNETOPAUSE; IMAGE OBSERVATIONS; X-LINE; MOTION; INTERPLANETARY; ACCELERATION; CLUSTER;
D O I
10.1002/2016GL069626
中图分类号
P [天文学、地球科学];
学科分类号
07 ;
摘要
Magnetic reconnection at the Earth's magnetopause is the primary process by which solar wind plasma and energy gains access to the magnetosphere. One indication that magnetic reconnection is occurring is the observation of accelerated plasma as a jet tangential to the magnetopause. The direction of ion jets along the magnetopause surface as observed by the Fast Plasma Instrument (FPI) and the Hot Plasma Composition Analyzer (HPCA) instrument on board the recently launched Magnetospheric Multiscale (MMS) set of spacecraft is examined. For those cases where ion jets are clearly discerned, the direction of origin compares well statistically with the predicted location of magnetic reconnection using convected solar wind observations in conjunction with the Maximum Magnetic Shear model.
引用
收藏
页码:5997 / 6004
页数:8
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