InterPlanetary Scintillation IPS induced Pluripotent Stem cell iPS.

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Presentation transcript:

InterPlanetary Scintillation IPS induced Pluripotent Stem cell iPS

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

Interplanetary Scintillation V & △ Ne

1964 Discovery of interplanetary scintillation Antony Hewish

1min

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

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

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 ㎡

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

Toyokawa Observatory SWIFT

Solar Wind Imaging Facility at Toyokawa 327 MHz EW40m×NS106m

a z Fresnel filter E Radio source weight

Radio source size E weight Radio source z a

Solar wind electron distribution ★ E E Sun weight Radio source

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

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

after Coles (1978) IPS vs. in situ

cross-correlation functions

Heliocentric Distance (Rs)Scintillation index

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

Major issues on solar wind

Complementary to spacecraft measurements

Ulysses First and only one Solar polar orbiter

bimodal Velocity gradient NS asymmetry

V B Plasma density distribution, IPS diffraction pattern

cross-correlation functions

VLA