1. InterPlanetary Scintillation IPS 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 Discovery of interplanetary scintillation Antony Hewish

5. 1min

6. 81.5 MHz 36000 m 2 Large aperture (high gain) antenna Short-time constant receiver

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

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

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. a z Fresnel filter E Radio source weight

13. Radio source size E weight Radio source z a

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

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

16. Fresnel filter ｚ o =2πa 2 /λ Radio source a/z o >θ z o =1 AU =1.5×10 8 km λ=1 m ⇒ a=150 km θ<0.2 arcsec

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

18. cross-correlation functions

19. Heliocentric Distance (Rs)Scintillation index

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

22. Major issues on solar wind

23. Complementary to spacecraft measurements

24. Ulysses First and only one Solar polar orbiter

26. bimodal Velocity gradient NS asymmetry

27. V B Plasma density distribution, IPS diffraction pattern

28. cross-correlation functions

29. VLA