HR: 0800h
AN: SH21B-0403    [Abstracts]
TI: Studying the Heliosphere with Long Time Series of Ulysses HISCALE Ion Composition Data
AU: * Thomson, D J
EM: djt@mast.queensu.ca
AF: Queens University, Dept of Math and Statistics 411 Jeffery Hall, Kingston, ON K7L 3N6 Canada
AU: Maclennan, C G
EM: cgm@lucent.com
AF: Bell Laboratories, Room 1E436, 600 Mountain Ave, Murray Hill, NJ 07974 United States
AU: Lanzerotti, L J
EM: ljl@lucent.com
AF: Bell Laboratories, Room 1E436, 600 Mountain Ave, Murray Hill, NJ 07974 United States
AU: Lanzerotti, L J
EM: ljl@lucent.com
AF: NJ Institute of Technology, Center for Solar-Terrestrial Research, Newark, NJ 07102 United States
AB: Ulysses has now been in orbit for fourteen years, over two full orbits and a full solar cycle. We take this opportunity to investigate the properties of long time series of ion composition data that have been acquired by the HI-SCALE instrument. We use daily average H and He fluxes measured by the Wart Pulse Height Analysis (PHA) system of HI-SCALE in the energy ranges of 0.35 MeV/nuc to 1.0 MeV/nuc for He/H ratios, and 0.5 to 2.0 MeV/nuc for species in the Z $>$ 2 composition range from Helium to Iron. Preliminary results show the expected dependence on solar cycle as well as on heliographic latitude of the spacecraft, and S/C distance from the Sun. We show the statistical relationship between He and H fluxes over this entire time interval (and sub time intervals), as well as between Z $>$ 2 ions and He fluxes. In addition, spectral analyses of the ln(He/H) flux ratios exhibit large spectral peaks (above 99% confidence levels at numerous frequencies. All the frequencies reported in the analyses of Thomson et al. (Nature, 1995) in the 0 to 5.8 uHz range are matched within 10 nHz at significance levels above 90% confidence. We suggest that the spectral peaks in the ion fluxes are evidence for the global oscillation (`breathing') of the heliosphere, where the driving source for the breathing is the Sun, i.e., solar oscillations. A 24 nHz fine-splitting visible on many of the lines suggests that the 1.38-year oscillation of the tachocline (Howe et al, Science, 2000) modulates the modes.
DE: 2114 Energetic particles, heliospheric (7514)
DE: 2118 Energetic particles, solar
DE: 2162 Solar cycle variations (7536)
DE: 2169 Sources of the solar wind
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting