HR: 1330h
AN: SH43A-11    [Abstracts]
TI: Origin of Heliospheric Magnetic Field Polarity Inversion at High Latitudes
AU: * Velli, M
EM: Marco.Velli@jpl.nasa.gov
AF: Jet Propulsion Lab., California Inst. of Technology, 4800 Oak Grove Dr, Pasadena, CA, CA 91109 United States
AU: Landi, S
AF: Dipartimento di Astronomia e Scienza dello Spazio, Universit† di Firenze, Largo E Fermi 2, Firenze, Fi 50125 Italy
AU: Hellinger, P
AF: Dipartimento di Astronomia e Scienza dello Spazio, Universit† di Firenze, Largo E Fermi 2, Firenze, Fi 50125 Italy
AU: Hellinger, P
AF: Institute of Atmospheric Physics, AS CR, Bocni II/1401, Prague, 14131 Czech Republic
AU: Winterhalter, D
AF: Jet Propulsion Lab., California Inst. of Technology, 4800 Oak Grove Dr, Pasadena, CA, CA 91109 United States
AB: High latitude observations of the magnetic field by the Ulysses spacecraft have shown a significance number of cases where the radial magnetic field polarity is reversed with respect to the dominant polarity of the coronal hole from which the wind emanates. Such reversals have the nature of folded back magnetic field lines. It has been suggested that such reversals are due to reconnection of closed and open field lines in the lower corona which would launch a large amplitude Alfvén wave into the solar wind. We suggested an alternative mechanism for the generation of the polarity reversal, namely, the coupling of standard large amplitude Alfvénic turbulence in the low frequency regime propagating away from the sun with the microstream shears observed in the high speed solar wind. Here we show that pressure and density signals are similiar to those observed in the data, and discuss the correlation of the reversals with the high latitude microstream structure.
DE: 2149 MHD waves and turbulence
DE: 2164 Solar wind plasma
DE: 7843 Numerical simulation studies
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly