Solar wind density structure at 1 AU and comparison to Doppler scintillation measurements

Details Solar wind density structure at 1 AU and comparison to Doppler scintillation measurements Solar wind density structure at 1 AU and comparison to Doppler scintillation measurements

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..530h&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 530

Computer Science

Solar Wind Plasma, Sources Of Solar Wind, Particle Emission, Solar Wind

Scientific paper

Results of a survey of solar wind density fluctuations in different flow types observed by ISEE-3 at 1 AU are presented and compared with Doppler scintillation measurements. We consider coronal hole, plasma sheet, interstream, CME and sheath interaction region flow types. For the quasi-stationary solar wind, densities (N) and density fluctuation levels (ΔN) are low in coronal hole flow, and high in the plasma sheet containing the heliospheric current sheet (HCS). The highest fluctuation levels are found in the sheath compression regions between CMEs and associated forward shocks. The streamer structure around the HCS broadens and erodes with distance from the Sun, and the broadened Doppler scintillation signature at 1 AU is in good qualitative agreement with ISEE-3 superposed epoch analysis. The observed asymmetry about the HCS is an expected result of solar wind dynamic evolution. A greater contrast between flow types is seen in ΔN levels rather than in N itself. Doppler scintillation responds to ΔN and thus provides a sensitive means of detecting interplanetary disturbances. However, we find that ΔN/N is not constant in the solar wind, and thus enhanced scintillation cannot unambiguously imply enhanced density.

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