Solar wind measured by interplanetary scintillation method
- Conference date: 5-9 Oct 1998
- Location: Nantucket, Massachusetts (USA)
Spacecraft observations of the solar wind have been confined to regions near the ecliptic plane until the Ulysses spacecraft has recently made a pass over both solar poles at a heliocentric distance of 2 to 4 AU (1) and encountered continuous fast wind at high latitudes, generally in a range of 700 to 800 km/s (2). On the other hand, there has been no direct measurement at solar distances inside where the solar wind is significantly accelerated. The interplanetary scintillation (IPS) method is a unique and useful means to measure global structure of the solar wind in regions near the Sun and at high latitudes where in situ measurements are difficult. Since the IPS measurements, however, are biased by line-of-sight integration effects, a computer assisted tomography method has been developed to deconvolve the line-of-sight integration. We introduce several results from the IPS tomography analysis on latitudinal velocity structure up to 90°, radial distance dependence of fast wind speed, origin of very slow wind, and density fluctuations.
- Solar wind
- Acceleration measurement
- Space vehicles
- Computer simulation
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