Physics
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21...85w&link_type=abstract
Geophysical Research Letters, vol. 21, no. 2, p. 85-88
Physics
16
Bandwidth, Electron Density (Concentration), Latitude, Mass, Radio Signals, Remote Sensing, Signal Distortion, Solar Corona, Solar Physics, Solar Wind Velocity, Sun, Superhigh Frequencies, Coronagraphs, Helios 1, Helios 2, Inference, Mariner 10 Space Probe, Mariner 4 Space Probe, Pioneer 10 Space Probe, Spacecraft Instruments, Variations, Velocity Measurement, Viking Spacecraft
Scientific paper
Spectral broadening measurements conducted at S-band (13-cm wavelength) during solar minimum conditions in the heliocentric distance range of 3-8 RO by Mariner 4, Pioneer 10, Mariner 10, Helios 1, Helios 2, and Viking have been combined to reveal a factor of 2.6 reduction in bandwidth from equator to pole. Since spectral broadening bandwidth depends on electron density fluctuation and solar wind speed, and latitudinal variation of the former is available from coherence bandwidth measurements, the remote sensing spectral broadening measurements provide the first determination of the latitudinal variation of solar wind speed in the acceleration region. When combined with electron density measurements deduced from white-light coronagraphs, this result also leads to the first determination of the latitudinal variation of mass flux in the acceleration region. From equator to pole, solar wind speed increases by a factor of 2.2, while mass flux decreases by a factor of 2.3. These results are consistent with measurements of solar wind speed by multi-station intensity scintillation measurements, as well as measurements of mass flux inferred from Lyman alpha observations, both of which pertain to the solar wind beyond 0.5 AU. The spectral broadening observations, therefore, strengthen earlier conclusions about the latitudinal variation of solar wind speed and mass flux, and reinforce current solar coronal models and their implications for solar wind acceleration and solar wind modeling.
Goldstein Richard M.
Woo Richard
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