On the causes of spectral enhancements in solar wind power spectra

Details On the causes of spectral enhancements in solar wind power spectra On the causes of spectral enhancements in solar wind power spectra

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976jgr....81..469u&link_type=abstract

Journal of Geophysical Research, vol. 81, Feb. 1, 1976, p. 469-482.

Astronomy and Astrophysics

Astronomy

6

Cross Correlation, Power Spectra, Radio Sources (Astronomy), Solar Wind Velocity, Bow Waves, Frequency Response, Graphs (Charts), Ionic Mobility, Ogo-5, Particle Flux Density, Shock Waves, Solar Corpuscular Radiation

Scientific paper

Enhancements in power spectra of the solar-wind ion flux in the frequency neighborhood of 0.5 Hz had been noted by Unti et al. (1973). It was speculated that these were due to convected small-scale density irregularities. In this paper, 54 flux spectra calculated from OGO 5 data are examined. It is seen that the few prominent spectral peaks which occur were not generated by density irregularities, but were due to several different causes, including convected discontinuities and propagating transverse waves. A superposition of many spectra, however, reveals a moderate enhancement at a frequency corresponding to convected features with a correlation length of a proton gyroradius, consistent with the results of Neugebauer (1975).

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