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

Sate

llites

SW

Paylo

ads

Geo.

Satellite

(GK2A)

MEMs,

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EASCO

Launch (2022)

500kg class

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(LEO)

GUVI and

WindII

CINEMA

/TRIO

KAIST

Small Sat.

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Corona

Graph for EASCO

500kg class

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(LEO)

Full disk Ha imaging

spectrograph

1000kg class

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