KASI Space Weather
Kyung-Suk ChoSpace Science Division
Korea Astronomy & Space Science Institute
KVN Yonsei Radio Astronomy Observatory
GPS Stations
KVN Ulsan Radio Astronomy Observatory
KVN Tamna Radio Astronomy Observatory
Daejeon
Seoul
KASI (Korea Astronomy & Space Science Institute)
About KASI - Organization
President
Vice-President
Audit Audit Division
Space Science Division
Optical Astronomy Division
Radio Astronomy Division
Planning Division
General Administration Division
Center for Large Telescope
Center for Theoretical Astronomy
Center for Small & Medium Enterprise Partnership
Office of Int’l & Public Relations
Center for Space Situational Awareness
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About Division - Organization
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Space Science Division
Group for Solar & Space Weather (28)
Group for Planetary Science (8)
Group for Space-based Astronomy (16)
Group for Space Geodesy (11)
Jae-Jin
Lee
Kyung-Suk
Cho
Young-Jun
Choi
Dae-Hee
Lee
Jungho
Jo
Hyung-Chul
Lim
Group for SLR (12)
02 KASI Space Weather
Research Center
Section
Solar Activity (CME, Flare, Type II)
SDORBSP
KSRBLNST
VHF radar
Space Weather
Prediction Center
Solar
Observation
Near-Earth Space Env.(Solar wind/Magnet./Iono.)
Sun-Earth Connection (CME geoeffectiveness)
Geomagnetic
Observation
Research
Projects Observations
SpaceWeatherCenter
Model and Service(Nowcast, Forecast, Alert)
Upper Atmospheric Observation
What we are doing
Infra
Observation system
DB &Network
Ground base
2007 2008 2009 2010 2011 2012 2013
Space(RBSP)
DB for ground infraSpace (SDO DB)
R&D
Basic research
Devel. of prediction
system
Devel. of service system Prediction/alert service
SWx effect
2015~
Operation of KASI
SW Research Center
Operation System operation
Ground base
SWx prediction
Roadmap for K-SWRC
2014
Summary of solar and SWR facilities
RBSP receiving antenna (Daejeon)
03 KASI SWx ResearchSection
Science Roadmap
Phase 1 Phase 2 Phase 3
2007 2008 2009 2010 2011 2012 2013 2014 2015 2016
Solar Activity
Magnetosphere
Ionosphere/ Thermosphere
NST Science
SDO Science
High Resolution study of Solar activity
CME Kinematics
Geoeffective CMEs
Relationship among CME-IP shock-Magnetosphere
Effects of CME & IP shock on Thermoshphre/Ionosphere
Coupling between magnetosphere & Ionosphere
RBSP Science
(Radiation Belt Storm Probe)Storm prediction based on CME
* NST(New Solar Telescope) * SDO(Solar Dynamics Observatory)
Coupling between upper atmosphere & lower atmosphere
Solar Telescope at BBSO
1.6m New Solar Telescope (NST)
Fast Imaging Solar Spectrograph (FISS)
World largest ground-basedoptical solar telescope
BBSO/UH/KASI/UA
SDO data center
• Data : 4K X 4K (IMAX quality) images, 1.5 TB/day
• Round-the-world high-performance network
• GLORIAD (GLObal RIng network for Advanced application Development)
GLORIAD
NASAMSOC, GSFC
ASIAData Center
※ KISTI (Korea Institute of Science and Technology Information)MSOC (Mission and Science Operations Center)
KASI SDO Website ( )
HAEBOGI (Viewer Software)
• Locational Offset• Normalized parameters
• Two equations for S and N MFOs
• Direction Parameter
• Empirical geomagnetic storm prediction model
Formula for predict the geomagnetic storm strength (Dst index)
• For southward events,
• For northward events,
G: KASI Geomagnetic Storm Forecast Model (Kim et al. 2010)
PODy PODn FAR Bias CSI
Empirical Model 0.93 0.50 0.26 1.25 0.70
• For 66 halo CMEs during solar cycle 23,
• ‘yes’ prediction is defined when our model predicts Dst ≤ -50 nT.
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① Propagating speed② Propagating direction③ Location and magnetic field orientation of
source region④ CME forecast table (Kim et al., 2010) Auto input and calculation
Direct measurement of parameters in web based system
- Speed, DP, MFO
KASI empirical forecast system for Geomagnetic Storms
• Prediction result - Storm time and strength- Probability
1 2
3
4
http://210.219.33.155/SEFRWeb/login/login.do
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RBSP receiving antenna
• RBSP, multi-satellite operation, provides useful data in understanding physics of Radiation Belts.
• RBSP receiving antenna was constructed at KASI in 2012 under corporation with NASA.
Research : Radiation belt study ( G 6-3)
Multiple harmonics upper hybrid waves in the radiation belt from EMFISIS instrument
Chorus wave
Plasma density from HOPE instrument & Energetic particles from MAGEIS instrument
Particle accelerations by chorus wave implemented to radial diffusion equation to predict energetic electrons’ flux
KASI VHF ionospheric radar
Daejeon36.18°N, 127.13°E(Dip lat. 26.70°N)
Operation start : December 29, 2009
Ionospheric E-region
irregularity
We have identified repeated occurrence of the FAIs at specific LT zones and classified them as continuous (morning), QP (nighttime), and afternoon FAIs.
Statistical result (Yang et al., 2015, JGR)
E-region FAIs has maximum occurrence rate in summer and minimum occurrence rate in spring.
(see P-24 in detail)
F-region post-sunset FAIs has largest occurrence rate in equinoxes, but the occurrence rate of the nighttime FAIs is largest in summer.
International Contributions
NST and NoRH operations are supported by KASI by 2018
Observations Using World Class Instrument
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Polar Upper Atmospheric Observations (Antarctic)
Terra Nova Bay(74°37’ S, 164 °12 ’E)
KASI plans to expand its observations to the polar upper
atmosphere by installing new instruments at Jang Bogo Station,
South Korea’s planned Antarctic station located in Terra Nova Bay
(74.37°N, 164.12°E).
We will install a GPS scintillation monitor and an all-sky camera
within this year.
Limitation- Lack of Scientific Understanding- Present SWx forecast is mainly based on statistical method.
Suggestions to AOSWA- Open basic research projects- S/W Contests- Session for AOSW Customers
The 3rd COSPAR Symposium
2013 2015 2017 2019 2021 20252023
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