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I nter P lanetary S cintillation IPS

I nter P lanetary S cintillation IPS. induced Pluripotent Stem cell i PS. What is the I nter P lanetary S cintillation (IPS)?. Why is the IPS a useful and powerful tool for space weather forecast?. I nter p lanetary S cintillation. V & △Ne. 1964

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I nter P lanetary S cintillation IPS

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  1. InterPlanetaryScintillationIPS induced Pluripotent Stem cell iPS

  2. What is the InterPlanetary Scintillation (IPS)? Why is the IPS a useful and powerful tool for space weather forecast?

  3. Interplanetary Scintillation V & △Ne

  4. 1964 Discoveryof interplanetary scintillation Antony Hewish

  5. 1min

  6. Large aperture (high gain) antenna • Short-time constant receiver 81.5 MHz 36000 m2

  7. 5 years later after IPS discovery IPS observations were begun in Japan.

  8. STEL Radiotelescope Array dedicated for IPS Observations Sugadaira Kiso • Data • Solar Wind Speed • Scintillation level (g-value) Aperture Size = ~ 2000or ~ 3400㎡ Frequency 327MHz Toyokawa Fuji

  9. STEL IPS Antennas as Viewed in Google Earth Fuji IPS Telescope (FIT) Kiso IPS Telescope (KIT)

  10. Toyokawa Observatory SWIFT

  11. Solar Wind Imaging Facility at Toyokawa 327 MHz EW40m×NS106m

  12. Fresnel filter a weight z E Radio source

  13. Radio source size a weight z Radio source E

  14. Solar wind electron distribution Sun ★ weight E Radio source E

  15. less weighted by radio source size effect and lower SW density Line of sight Highest SW density less weighted by Fresnel filter and lower SW density

  16. Fresnel filter 　ｚo=2πa2/λ Radio source a/zo>θ zo=1 AU =1.5×108 km λ=1 m ⇒ a=150 km θ<0.2 arcsec

  17. IPS vs. in situ after Coles (1978)

  18. cross-correlation functions

  19. Scintillation index Heliocentric Distance (Rs)

  20. It can observe the near Sun region. Interplanetary Scintillation It can observe high latitude regions. It has wide spatial coverage of 3D space. It can observe vast space in a short time. Complementary observations to spacecraft

  21. Major issues on solar wind

  22. Complementary to spacecraft measurements

  23. Ulysses First and only one Solar polar orbiter

  24. NS asymmetry Velocity gradient bimodal

  25. V B Plasma density distribution, IPS diffraction pattern

  26. cross-correlation functions

  27. VLA

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