Space Weather Activities in KASI
Yeon-Han Kim
Space Science Division(SSD)
Korea Astronomy and Space Science Institute(KASI)

Outline

IIntroduction

II

Instrument Construction

III

Space Weather Researches

IVSpace Weather Monitoring System

V

Future PlansⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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SSD in KASI• For solar physics and space weather research, KASI
is the leading institute in Korea.
• The division is in charge of solar physics and space
weather research in KASI and the development andmanagement of related instruments.
• Originally, KASI has 3 optical solar observing
facilities; Solar Sunspot Telescope (SST, since 1987),
Solar Flare Telescope (SOFT, since 1995), and KASI
Solar Imaging Spectrograph (KSIS, since 2002).
• Since 2004, we have participated in the developmentof 1.6 meter New Solar Telescope (NST) in USA anddeveloped Korean Solar Radio Burst Locator(KSRBL) in cooperation with NJIT.
Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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SSD in KASI
Solar Activity(CME, flare, Type II)

Sun-Earth Connection(CME geoeffectiveness)

Near-Earth Space Env.
(Solar wind/Magnet./Iono.)

ResearchSolar
Observation

NSTSolar/SpaceWeather
CenterK-SRBL
ProjectsSpace Weather
Prediction CenterObservations

Model and Service(Nowcast, Forecast, Alert)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

IonosphericObservation

Geomagnetic
Observation4

Major Projects and Budget

Projects
Construction of space weather prediction center(space weather project)

Annual Budget inaverage$1.5 M

Study on effects of CMEs and high-speed solar
wind in the near-Earth space$0.2 M(leading research project)
Operation of solar observation systems(instrument operation project)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

$0.2 M

5Roadmap for K-SWPCⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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Science Roadmap
Phase 2Phase 1
2007200820092010

2011

Phase 32012

2013

2014

2015

2016

CME Kinematics
Geoeffective CMEs
Solar Activity
NST Science

High Resolution studyof Solar activity

SDO Science

Magnetosphere

Ionosphere/Thermosphere

Relationship among CME-IP
shock-Magnetosphere

RBSP Science

Storm prediction based on CME(Radiation Belt Storm Probe)

Effects of CME & IP shock on
Thermoshphre/Ionosphere* NST(New Solar Telescope)

Coupling between
magnetosphere & Ionosphere* SDO(Solar Dynamics Observatory)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

7II. Instrument Construction▣ SWML (2007): space weather monitoring▣ e-CALLISTO (2007): solar radio burst, spectrum▣ Magnetometers: geo-magnetic fieldv Fluxgate (2007), Proton (2009), MI sensors (2009)▣ All Sky Imager (2008): ionosphere, optical (97, 250km)▣ SCINTMON (2008): ionosphere, scintillation▣ KSRBL (2009): solar radio burst, spectrum, sourcelocation▣ VHF Radar (2009): ionosphere E-, F-layerirregularity▣ 1.6m NST: world largest ground-based opticalsolar telescope (photosphere, chromosphere)v CT (2009), FISS (2010)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Instrument LocationⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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Korean Solar Radio Burst Locator (KSRBL)
Korean Solar Radio Burst
Locator (KSRBL) is a single
dish radio spectrograph,
which has been developed incollaboration with New Jersey
Institute of Technology andinstalled at KASI in August
2009. KSRBL records thespectra of solar microwave
bursts with high time andfrequency resolution, andlocates their positions on thesolar disk.
Frequency range

245,410MHz , 0.5-18GHz

Frequency
resolution

1MHzTime resolution

1sLocation accuracy

0.03°Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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FISS (Fast Imaging Solar Spectrograph)

NasmythⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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FISS Observation# NST-Hinode joint obs.
Oct. 26 2010

Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

Oct. 27 201012

III. KASI Space Weather Researches▣ CMEs geoeffectivenessv Forecast of geoeffective CMEs
v Earthward direction of CMEs

▣ Empirical relationship between CMEs initial speedand solarwind dynamic pressure▣ IP shock propagation model▣ High resolution study of solar activities
v Small pores, spicule oscillations, solar tornado▣ Satellite drag during strong solar andgeomagnetic activities▣ Satellite anomalies due to space weather effect▣ High lat. thermospheric density depending on IMF▣ Auroral observation by STSAT-1Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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CME geoeffectiveness

Q

What CME parameters control geomagnetic storms ?
How can you estimate the probability to produce ageomagnetic storm ?

ASpeedLocationDirectionⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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Forecast of geoeffective CMEs (I. Speed & Location)
Combinationof Location and Speed• Probability map of the CME geoeffectiveness (Dst < -50nT)–

The high probability area becomes wider for fast CMEs–

Third criterion : for fast CME (≥ 800km/s), -30 < Lon. < +60for slow CME (< 800km/s), 0 < Lon. < +30

Speed (Km/s)
1200

800

400-60(East)

-30

030
Longitude (degree)

60(West)(R. S. Kim et al. 2005)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Earthward Direction of CMEs
We propose a new quantitative direction parameter !
▣ Degree of symmetry : (b/a)

abb/a = 0.64

• 86% (161/188) of geoeffective CMEs havelarge direction (D ≥ 0.4)
• CMEs with large D are more geoeffective
than fast CMEs

(Moon et al. 2006)(R. S. Kim et al. 2008)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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IV. Space Weather Monitoring System (2007~)Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Contents of SWMS
1. Observational data from oversea and domestic
2. Shock propagation modelsvEmpirical models for shock arrival time

3. Geomagnetic storm forecastv

CME initial speed, source location, direction para. ->probability forecast for geomag. storm occurrence

4. Solarwind predictionv

Coronal hole information -> solarwind information

5. Space weather monitoring for GEO sat.
v

Magnetopause monitor, satellite anomaly region, meteor
information, etc.

6. Space weather monitoring for polar route flightv

Information for high E. ptcls. & communicationⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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V. Future Plans▣ KASI-NASA collaboration (LOA, 2010)
To obtain the real-time space weather data from satellite obs.
2. SDO data center• Storage (1.5TB/day)• Data analysis server• Gloriad (inter-cont. network)• Real-time monitoring
1.

3.

RBSP receiving station• Antenna (6m)
• Receiver• Data server• Real-time monitoringⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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SDO, Solar Dynamics Observatory

Launched on 11 February 2010

Solar and Astrophysics Lab

Helioseismic andMagnetic Imager

EUV VariabilityExperimentAtmospheric Imaging
Assembly20

Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Why should KASI construct KDC for SDO?

▣For solar and space weather researchv High cadence and high resolution data

▣Very large data sizev It is not easy to successfully download large

scientific data of SDO from NASA.
v It is totally impossible through public network.

▣For space weather applications
v Realtime or quasi realtime SDO data

Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Data Centers for SDO

KDC for SDO
KASI , Korea

UCLan,United Kingdom

SDO at SIDC
ROB, Belgium

JSOC (AIA and HMI)
Stanford Univ. andLMSAL, USAIAS,France

EVE
Univ. of Colorado
at Boulder, USA
Full Data

GDC for SDO
DLR, Germany

Short-term andSelected Data

DLR, Deutsches Zentrum für Luft- und Raumfah KDC, Korean Data Center(German Aerospace Center)
LMSAL, Lockheed Martin Solar and Astrophysics Lab
GDC, German Data Center
ROB, Royal Observatory of Belgium
IAS, Institut d'Astrophysique Spatiale
SIDC, Solar Influences Data Center
JSOC, Joint Science Operations Center
UCLan, University of Central LancashireⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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GLORIAD24

The Radiation Belt Storm Probes (RBSP)▣ NASA will launch two identical probes into the radiation belts to provide
unprecedented insight into the physical dynamics of near-Earth space.
▣ The radiation belts are now part of our technology infrastructure.
v If we can understand the belts, we can improve our mission planning, and spacecraft operation and system design▣ Data collected by the probes will help researchers develop and improvevarious models for the radiation belts that can be used by:– engineers to design radiationhardened spacecraft– forecasters to predict space weather phenomena and alert
astronauts and spacecraft operators to potential hazards– spacecraft operators for ano
maly resolution

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RBSP Mission Summary▣2 Near-Sun Pointing Observatories▣Spin Stabilized ~5 RPM▣Spin-Axis 15°-27° of Sun▣Operational Design Life of 2 years (additional propellant will be
carried to allow for extended mission

Perigee Altitude 625 km
Inclination 10°

Differing apogees allow for simultaneous
measurements to be taken over the full range ofobservatory separation distances several times overthe course of the mission. This design allows
Observatory 2 to lap Observatory 1 every 79 days.

Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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S-band 7m Antenna assembly in KASI

Korean RBSP receiving station started to construct
last month and will be completed before June 2012.
Ⓒ Korea Astronomy and Space Science Institute. All rights reserved.

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Thank youⒸ Korea Astronomy and Space Science Institute. All rights reserved.

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