Abstract. EISCAT observations of interplanetary scintillation have been used to measure the velocity of the solar wind at distances between 15 and 130 R � (solar radii) from the Sun. The results show that the solar wind consists of two distinct components, a fast stream with a velocity of &800 k...
| Main Authors: | , , |
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| Other Authors: | |
| Format: | Text |
| Language: | English |
| Published: |
1996
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| Online Access: | http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.371.7543 http://hal.archives-ouvertes.fr/docs/00/31/62/44/PDF/angeo-14-1235-1996.pdf |
| Summary: | Abstract. EISCAT observations of interplanetary scintillation have been used to measure the velocity of the solar wind at distances between 15 and 130 R � (solar radii) from the Sun. The results show that the solar wind consists of two distinct components, a fast stream with a velocity of &800 km s� � and a slow stream at &400 km s��. The fast stream appears to reach its final velocity much closer to the Sun than expected. The results presented here suggest that this is also true for the slow solar wind. Away from interaction regions the flow vector of the solar wind is purely radial to the Sun. Observations have been made of fast wind/slow wind interactions which show enhanced levels of scintillation in compression regions. 1 |
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