HR: 11:35h
AN: SH42A-06    [Abstracts]
TI: The relation between the solar wind dynamic pressure at Voyager 2 and the energetic particle events at Voyager 1
AU: * richardson, j d
EM: jdr@space.mit.edu
AF: Center for Space Research, Massachusetts Institute of Technology, MIT 37-555, cambridge, ma 02139 United States
AU: McDonald, F B
EM: fm27@umail.umd.edu
AF: Institute for Physical Science and Technology, University of Maryland, College Park, md 20742-2431 United States
AU: Stone, E C
EM: ecs@srl.caltech.edu
AF: Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, ca 91125 United States
AU: Wang, C
EM: cw@space.mit.edu
AF: Center for Space Research, Massachusetts Institute of Technology, MIT 37-555, cambridge, ma 02139 United States
AU: Wang, C
EM: cw@space.mit.edu
AF: Center for Space Science and Applied Research, Chinese Academy of Sciences, P.O. Box 8701, Beijing, 100080 China
AB: Voyager 1 energetic particle data suggest the recent close approach to, or crossing of, the termination shock. Although the plasma experiment on Voyager 1 is not providing useful data, plasma data from Voyager 2 may shed light on the plasma conditions at Voyager 1. Before the first particle event, Voyagers 1 and 2 see similar particle signatures. Voyager 2 pressure and energetic particle flux profiles have similar structure. Changes in the energetic particle flux at Voyager 1 are associated with merged interaction regions (MIRs) passing the spacecraft. Many MIRs are observed at both spacecraft, so Voyager 2 dynamic pressures may predict energetic particle changes at Voyager 1 and the movement of the termination shock near Voyager 1. The magnetic field strength and dynamic pressure are correlated at Voyager 2 so that changes in the magnetic field strength may serve as a proxy for dynamic pressure changes at Voyager 1.
DE: 2104 Cosmic rays
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2114 Energetic particles, heliospheric (7514)
DE: 2124 Heliopause and solar wind termination
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting