Observing the Solar Wind with Interplanetary Scintillation
Observing the Solar Wind with Interplanetary Scintillation Observing the Solar Wind with Interplanetary Scintillation
Coronal Mass Ejections (CMEs) ● Presence of CME can be indicated by different features: ● ● ● Substantial changes in form of crosscorrelation function Sudden increase in scintillation level Negative lobe on cross-correlation function. Large “negative lobe” indicates magnetic field rotation
Longer Baselines If longer baselines are used, cross-correlation function may show multiple peaks. Peaks correspond to different solar wind streams.
- Page 1 and 2: Observing the Solar Wind with Inter
- Page 3 and 4: Radio Measurements Line of sight to
- Page 5: Cross-Correlation Cross-correlation
- 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
Longer Baselines<br />
If longer baselines are<br />
used, cross-correlation<br />
function may show multiple<br />
peaks.<br />
Peaks correspond to<br />
different solar wind<br />
streams.
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