Observing the Solar Wind with Interplanetary Scintillation
Observing the Solar Wind with Interplanetary Scintillation Observing the Solar Wind with Interplanetary Scintillation
Radio Source Tracking Difference between maximum and minimum levels Movement of main source Side Lobe Movement of strong source Movement of the source within the main beam is negligible, but strong source Main Peak in a sidelobe could modulate the signal by the slewing frequency of 0.39Hz
Filter Settings Power Central Filter Frequencies Frequency • Signal passes through a rack of six channel boards. • Filters on these boards are used to sample different parts of the signal. • For IPS, these filters are set to 1.8MHz wide with central frequencies such as to cover a bandwidth of 5.4MHz. We can/could only use three channel boards: Data rate too high for more!
- Page 1 and 2: Observing the Solar Wind with Inter
- Page 3 and 4: Radio Measurements Line of sight to
- Page 5 and 6: Cross-Correlation Cross-correlation
- 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: Radio Source Tracking ● ● ●
- Page 19 and 20: Median Sampling ● ● Data usuall
- Page 21 and 22: 1420MHz System
- Page 23: Summary ● EISCAT used for observi
Radio Source Tracking<br />
Difference between<br />
maximum and<br />
minimum levels<br />
Movement of<br />
main source<br />
Side Lobe<br />
Movement of<br />
strong source<br />
Movement of <strong>the</strong> source<br />
<strong>with</strong>in <strong>the</strong> main beam is<br />
negligible, but strong source<br />
Main Peak<br />
in a sidelobe could modulate<br />
<strong>the</strong> signal by <strong>the</strong> slewing<br />
frequency of 0.39Hz
Change language