Observing the Solar Wind with Interplanetary Scintillation
Observing the Solar Wind with Interplanetary Scintillation Observing the Solar Wind with Interplanetary Scintillation
The Sun's Atmosphere The Solar Corona (March 2006 eclipse). The Solar Wind: Expansion at supersonic speeds of the Corona through the solar system. Often two streams: “Fast” at ~750km/s and “slow” at ~350km/s. Space Weather: The impact of the solar wind and solar events such as Coronal Mass Ejections on the Earth's magnetic field and ionosphere.
Radio Measurements Line of sight to radio source Scintillation due to turbulent-scale density variations in the Solar Wind Time Lag ● Simultaneous measurements by two antennas show similar patterns of scintillation. ● Time-lag for maximum cross-correlation gives estimate of solar wind outflow speed.
- Page 1: Observing the Solar Wind with Inter
- 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 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
The Sun's Atmosphere<br />
The <strong>Solar</strong> Corona (March 2006 eclipse).<br />
The <strong>Solar</strong> <strong>Wind</strong>: Expansion at supersonic speeds<br />
of <strong>the</strong> Corona through <strong>the</strong> solar system. Often two<br />
streams: “Fast” at ~750km/s and “slow” at ~350km/s.<br />
Space Wea<strong>the</strong>r:<br />
The impact of <strong>the</strong> solar wind<br />
and solar events such as<br />
Coronal Mass Ejections on <strong>the</strong><br />
Earth's magnetic field and<br />
ionosphere.
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