Halo coronal mass ejections (CMEs) originating from solar activities give rise to geomagnetic storms when they reach the Earth. Variations in the geomagnetic field during a geomagnetic storm can damage satellites, communication systems, electrical power grids, and power systems, and induce currents. Therefore, automated techniques for detecting and analyzing halo CMEs have been eliciting increasing attention for the monitoring and prediction of the space weather environment. In this study, we developed an algorithm to sense and detect halo CMEs using large angle and spectrometric coronagraph (LASCO) C3 coronagraph images from the solar and heliospheric observatory (SOHO) satellite. In addition, we developed an image processing technique to derive the morphological and dynamical characteristics of halo CMEs, namely, the source location, width, actual CME speed, and arrival time at a 21.5 solar radius. The proposed halo CME automatic analysis model was validated using a model of the past three halo CME events. As a result, a solar event that occurred at 03:38 UT on Mar. 23, 2014 was predicted to arrive at Earth at 23:00 UT on Mar. 25, whereas the actual arrival time was at 04:30 UT on Mar. 26, which is a difference of 5 hr and 30 min. In addition, a solar event that occurred at 12:55 UT on Apr. 18, 2014 was estimated to arrive at Earth at 16:00 UT on Apr. 20, which is 4 hr ahead of the actual arrival time of 20:00 UT on the same day. However, the estimation error was reduced significantly compared to the ENLIL model. As a further study, the model will be applied to many more events for validation and testing, and after such tests are completed, on-line service will be provided at the Korean Space Weather Center to detect halo CMEs and derive the model parameters.

1. INTRODUCTION
 2. AUTO-DETECTION PROCESS FOR HALO CME
 3. ALGORITHM FOR MORPHOLOGICAL ANDMECHANICAL PROPERTIES OF HALO CME
  3.1 Image Processing Technique for Characteristic Factors
  3.2 Development of CAT 3-D Parameter Program
 4. VERIFICATION OF CME PARAMETERS AS THEINPUTS OF SOLAR WIND PROPAGATION MODEL
  4.1 Halo CME Event Selection
  4.2 Test Results
 5. CONCLUSIONS
 ACKNOWLEDGMENTS
 REFERENCES

• Kyu-Cheol Choi(SELab Inc., Seoul 06049, Korea) Corresponding Author
• Mi-Young Park(SELab Inc., Seoul 06049, Korea)
• Jae-Hun Kim(Korean Space Weather Center, National Radio Research Agency, Jeju 63025, Korea)