Spectra of Ulysses {HISCALE} Electrons, 2001

Details Spectra of Ulysses {HISCALE} Electrons, 2001 Spectra of Ulysses {HISCALE} Electrons, 2001

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh11a0379t&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH11A-0379

Physics

7514 Energetic Particles (2114), 7522 Helioseismology, 7807 Charged Particle Motion And Acceleration

Scientific paper

Fluxes of low-energy ( ~50 - 200 keV) electrons during Ulysses' solar south pole to north solar pole pass in 2001 were of sufficient magnitude to compute reliable power spectra in the frequency range where low-order and degree g- and p- solar oscillatory modes are expected. In the 100 to 1000 μHz frequency range the spectra are dominated by large peaks that are reproducible between different electron flux and energy channels. Moreover, almost all of these peaks correspond to predicted mode frequencies for 0 <= l <= 5 to within a few microhertz, although there appear to be some systematic differences between predictions and observations. Several of the large peaks in the spectra are sufficiently isolated in frequency to allow hypothesis tests for spherical harmonic dependence in heliographic latitude. (The spacecraft's motion means that space and time are confounded so that one cannot reliably detect modes by simply testing for periodic components. Instead, one must include the amplitude and phase changes expected for a given mode along the orbit.) Preliminary tests using narrow band filters on some tentatively identified modes show the expected amplitude and phase characteristics.

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