IMAGE-Cluster Science Synergy

T.E. Moore (1), J.L. Burch (2), H.U. Frey (5), S.A. Fuselier (3), D.L. Gallagher (4), 
J. Green (1), S. Mende (5), D. G. Mitchell (6), W. Sandel (7), C.J. Pollock (2), 
B. Reinisch (8)

(1) NASA Goddard Space Flt. Ctr, Greenbelt MD USA
(2) Southwest Res. Inst., San Antonio, TX USA
(3) Lockheed Martin Adv. Tech. Ctr., Palo Alto, CA USA
(4) NASA Marshall Space Flt Ctr., Huntsville, AL USA
(5) Univ. Calif. Berkeley, CA USA
(6) Johns Hopkins U., Laurel MD USA
(7) U. Arizona, Tucson AZ USA
(8) U. Mass., Lowell, MA USA


A fortuitous aspect of the delay of the ESA Cluster Mission is that IMAGE and Cluster 
are now flying together, complementing each other as magnetospheric macroscope and 
microscope, respectively. IMAGE provides global to mesoscale context observations, 
while Cluster provides a high resolution in situ probe of conditions within the 
imaging space of IMAGE. In this paper, we describe some of the IMAGE observations 
that provide context for in situ observations from Cluster. These include ENA and RPI 
observations of the dayside solar wind interaction with the magnetosphere; ENA 
imaging of ionospheric heating and outflow, of plasma sheet injection into the ring 
current, and of ring current development and decay; FUV imaging of auroral 
development in substorms and storms; EUV observations of dynamic inner magnetospheric 
plasma flows; and RPI observations of magnetospheric plasma boundaries and their 
dynamics. Conversely, we describe some of the Cluster observations that help to 
diagnose processes that influence the global distribution of magnetospheric plasmas 
and their precipitation patterns. These include CIS, Peace, and RAPID observations of 
solar and ionospheric plasma populations at high altitudes near the magnetopause and 
in the magnetotail, FGM, EFW, and EDI observaitons of electric and magnetic fields 
during substorm and storm events, and WHISPER, WBD, DWP, and STAFF observations of 
waves and field fluctuations in association with events and boundary regions.

_______________
Presented at the 34th COSPAR Scientific Assembly, Houston, Texas, U.S.A.  
10-19 October 2002