HR: 16:15h
AN: SH34A-04    [Abstracts]
TI: Signatures of Differential Rotation in Low-Frequency Spectra of Heliospheric Fields
AU: * Roberts, D A
EM: aaron.roberts@nasa.gov
AF: NASA Goddard Space Flight Center Laboratory for Solar and Space Physics, Code 612.2, Greenbelt, MD 20771 United States
AU: Giacalone, J
EM: giacalon@lpl.arizona.edu
AF: University of Arizona, Department of Planetary Sciences, Tucson, AZ 85721-0092 United States
AU: Jokipii, R
EM: jokipii@lpl.arizona.edu
AF: University of Arizona, Department of Planetary Sciences, Tucson, AZ 85721-0092 United States
AU: Goldstein, M L
EM: melvyn.l.goldstein@nasa.gov
AF: NASA Goddard Space Flight Center Laboratory for Solar and Space Physics, Code 612.2, Greenbelt, MD 20771 United States
AB: We use Ulysses data to examine low-freqeuncy power spectra of the components and magnitude of the solar wind magnetic and velocity fields to search for signatures of photospheric differential rotation. Previous work has shown evidence for both the rigid coronal hole rotation period and for the photospheric rotation period associated with the likely source region of the fast wind at high latitidue. Here we show that while the differential rotation is seen in"compressive" quantities such as the magnitude of the magnetic field and density, the components of the field tend not to show the same differential rotation period peaks. Comparing the results to predictions of a version of the "Fisk field" model, while not ruling out the model, raises important questions about the explanations for rigid coronal hole rotation. We will discuss various alternative scenarios.
DE: 2134 Interplanetary magnetic fields
DE: 2164 Solar wind plasma
DE: 2169 Sources of the solar wind
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly