The Automatic Solar Synoptic Analyzer (ASSA) is a fully automated software system of realtime monitoring and identification of key solar phenomena such as sunspot groups, coronal holes and filaments, those are three major solar sources causing the space weather.
ASSA uses highresolution SDO HMI continuum and magnetogram data as inputs and identifying sunspot groups and providing McIntosh classification and Mt. Wilson magnetic classification of each active region. The pipeline of procedures for ASSA system include various kinds of image processing techniques including algorithms for intensity thresholding, morphological open/close, region growing and grouping based on the separation of each sunspot. Afterwards, each identified sunspot group is further processed to determine its McIntosh and Mt. Wilson magnetic class through estimation of quantitative parameters such as existence and maturity of penumbra, longitudinal coverage extent, compactness of sunspots aggregation, complexity of magnetic neutral lines, etc. The basic theory of classification scheme is based on SIDC user guide on sunspot group classification.
The flare probabilities for C/M/X class are provided. The C/M/X flare probabilities are based on the result of statistical analysis of the ASSA sunspot catalog and GOES Xray flare data. In generating the ASSA sunspot catalog, the SOHO MDI Continuum and Magnetogram images were collected for the period about 15 years from September 1996 to January 2011, which is covering a complete solar cycle (the cycle 23). Then, ASSA algorithm has been applied to the whole data set to obtain 15year sunspot catalog based on ASSA. The result of McIntosh classification for all sunspot groups are associated with Xray events catalog to yield C/M/X flare probability for each McIntosh class.
When identifying coronal holes and filament channels, images of SDO AIA 193 and global Halpha network are used for morphological identification. Especially, SDO HMI magnetograms are also used for quantitative verification of coronal hole based on polarity distribution. The output results of ASSA are routinely checked and validated against NOAA's daily SRS (Solar Region Summary) and UCOHO
This software was developed at the Korean Space Weather Center of the Radio Research Agency by SELab, Inc. This software is a freeware. It is an experimental system and RRA assumes no responsibility whatsover for its use by other parties, and make no guarantees.
SDO HMI continuum
SDO HMI magnetogram
SDO AIA 193
GONG Halpha (BBSO)
GONG Halpha (Udaipur)
Solar Region Summary from SWPC
UCOHO (URSIgram code for coronal hole information) from SWPC
Image and text files of sunspot identification and classification result according to McIntosh and Mt. Wilson classification scheme along with flare probability according to McIntosh sunspot classification results
Image and text files of coronal hole identification results
Image and text files of filament channel identification results
- Bloomfield, D. S., Higgins, P. A., McAteer, R. T. J., Gallagher, P. T., ApJL, 747, L41, 2012
- Colak, T., and Qahwaji, R., Solar Physics, 248, 277, 2007
- Krista, L. D. and Gallagher, P. T., Solar Physics, 256, 87, 2009
- Shih, F. Y. and Kowalsky, A. J., Solar Physics, 218, 99, 2003
Code Languages: IDL
- Jaehun Kim, Korean Space Weather Center (Model Contact)
- Sandro Taktakishvili, NASA GSFC CCMC (CCMC Model Host)
- M Leila Mays, NASA GSFC CCMC (CCMC Model Host)
- Peter MacNeice, NASA GSFC CCMC (CCMC Model Host)
In addition to any model-specific policy, please refer to the General Publication Policy.