Observing the Solar Wind with Interplanetary Scintillation
Observing the Solar Wind with Interplanetary Scintillation Observing the Solar Wind with Interplanetary Scintillation
Scintillation Index - “g-level” Plot courtesy P.K. Manoharan After Coles, 1978 ● ● Scintillation index is basic measure of the amount of scintillation: ● g-level is index normalised for distance: Can be related to solar wind density. Peak at certain distance: ● ● “Strong” scattering closer to the Sun; “Weak” scattering further away. Distance of peak depends on observing frequency'.
Cross-Correlation Cross-correlation function of time series from two stations shows peak at time-lag. First estimate of solar wind speed.
- Page 1 and 2: Observing the Solar Wind with Inter
- Page 3: Radio Measurements Line of sight to
- Page 7 and 8: Longer Baselines If longer baseline
- Page 9 and 10: Tomography ● Many observations ta
- Page 11 and 12: Tomography Co-rotating analysis Com
- Page 13 and 14: Why EISCAT? ● ● ● ● Observi
- Page 15 and 16: Radio Source Tracking ● ● ●
- Page 17 and 18: Filter Settings Power Central Filte
- Page 19 and 20: Median Sampling ● ● Data usuall
- Page 21 and 22: 1420MHz System
- Page 23: Summary ● EISCAT used for observi
<strong>Scintillation</strong> Index - “g-level”<br />
Plot courtesy P.K. Manoharan<br />
After Coles, 1978<br />
●<br />
●<br />
<strong>Scintillation</strong> index is basic measure of <strong>the</strong> amount of scintillation:<br />
●<br />
g-level is index normalised for distance: Can be related to solar wind density.<br />
Peak at certain distance:<br />
●<br />
●<br />
“Strong” scattering closer to <strong>the</strong> Sun; “Weak” scattering fur<strong>the</strong>r away.<br />
Distance of peak depends on observing frequency'.
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