HR: 10:55h
AN: SH41D-03    [PDF]
TI: Nature of the Plasma Sheet Between Same-Polarity Solar Wind Streams
AU: Neugebauer, M
EM: mneugeb@cox.net
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive Mail Stop 169-506, Pasadena, CA 91109 United States
AU: Neugebauer, M
EM: mneugeb@cox.net
AF: University of Arizona, Lunar and Planetary Laboratory, Tucson, AZ 85721 United States
AU: Zhou, X
EM: Xiaoyan.Zhou@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive Mail Stop 169-506, Pasadena, CA 91109 United States
AU: * Goldstein, B E
EM: Bruce.Goldstein@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive Mail Stop 169-506, Pasadena, CA 91109 United States
AU: Liewer, P C
EM: Paulett.Liewer@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive Mail Stop 169-506, Pasadena, CA 91109 United States
AU: Steinberg, J T
EM: jsteinberg@lanl.gov
AF: Los Alamos National Laboratory, Mail Stop D466, Group NIS-1, Los Alamos, NM 87545 United States
AB: Heliospheric spacecraft occasionally encounter consecutive high-speed streams that map to two different solar source regions with the same magnetic polarity. The low-speed wind between the two streams has many similarities to the plasma sheets commonly observed between high-speed streams, except that there is no current sheet. We have studied several such plasma sheets observed with the Ulysses spacecraft during the fast, pole-to-pole latitude scans in 1995 and 2001 and with ACE. Common features are large amplitude tangential discontinuities, regions of low entropy, some very low helium abundances, and magnetic holes.
DE: 2102 Corotating streams
DE: 2109 Discontinuities
DE: 2162 Solar cycle variations (7536)
DE: 2169 Sources of the solar wind
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting