HR: 14:10h
AN: SH12B-03 INVITED     [PDF]
TI: Evidence That Voyager 1 Exited the Solar Wind at $\sim$85 AU and Re-entered at $\sim$87 AU in August 2002 and February 2003.
AU: * Krimigis, S M
EM: tom.krimigis@jhuapl.edu
AF: Applied Physics Laboratory, The Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD 20723 United States
AU: Decker, R B
EM: rob.decker@jhuapl.edu
AF: Applied Physics Laboratory, The Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD 20723 United States
AU: Hill, M E
EM: mehill@umd.edu
AF: Department of Physics, University of Maryland, College Park, MD 20742 United States
AU: Roelof, E C
EM: edmond.roelof@jhuapl.edu
AF: Applied Physics Laboratory, The Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD 20723 United States
AU: Armstrong, T P
EM: armstrong@ftecs.com
AF: Fundamental Technologies, 2411 Ponderosa, Suite A, Lawrence, KS 66046 United States
AU: Gloecker, G
EM: gg10@umail.umd.edu
AF: Department of Physics, University of Maryland, College Park, MD 20742 United States
AU: Hamilton, D C
EM: douglas.c.hamilton@umail.umd.edu
AF: Department of Physics, University of Maryland, College Park, MD 20742 United States
AU: Lanzerotti, L J
EM: ljl@lucent.com
AF: Bell Laboratories, 600 Mountain Avenue, Building 1E-439, Murray Hill, NJ 07974 United States
AU: Lanzerotti, L J
EM: ljl@lucent.com
AF: Center for Solar Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07102 United States
AB: The LECP instrument on V1, V2 consists of a collection of solid-state detectors designed to perform measurements of ions ($\sim$30keV to 10s of MeV) and electrons ($\sim$28 keV to $\sim$10 MeV), including elemental composition over a range of energies ($_{\_>}$0.3 MeV/nuc) and species (H, He, C, N, O, Ne, etc). Salient features of the observations during 2002-2003 are as follows: (a) A gradual increase in $\sim$1 MeV proton intensity in late 2000 culminated in an 100-fold step increase in mid-2002 lasting for $>$6 months and ending within a few hours in early 2003. (b) The step increase was seen in energies ranging from $\sim$40 keV to $>$70 MeV for protons and $>$0.35 MeV for electrons. (c) Large intensity fluctuations lasting from $<$1 to several days were present coherently in all energies and species throughout the period. (d) The composition of H, He, O and C are consistent with an ACR or PUI source. (e) Outward streaming anisotropies show that the particle source lies inside the V1 location. (f) Generalized (non-linear) Compton-Getting fits to the angular distributions show the convection velocity changed from 300 km/s to $<$50km/s and back to $\sim$230km/s before, during, and after the increase, respectively. Post-re-entry observations show frequent inward and some outward proton flows, suggesting a significant radial component of the IMF. The observations will be discussed in the context of current theoretical models of the interaction between the heliosphere and the local interstellar medium.
DE: 2124 Heliopause and solar wind termination
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting