Sol

Solar Flare Monitor

ASAP Flare Monitor Image


Update Interval: 240 min.

Internal name: asap_flare_monitor_image
Cygnet Description: Automated Solar Activity Prediction (a.k.a ASAP) is a system to predict solar flares and CMEs in near real-time. ASAP currently works for flare prediction and further work on CMEs continues.


Coronal Holes

ASSA Detected Coronal Holes Plot


Update Interval: 60 min.

Internal name: ASSA Detected Coronal Holes Plot
Cygnet Description: ASSA-detected coronal holes plot based on SDO AIA 193.

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.
It is provided by the Korean Space Weather Center of National Radio Research Agency.
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.


Active Regions

Active regions (JSOC/Stanford)


Update Interval: 60 min.

INFO: The image shows the full-disk line-of-sight magnetic fields from the Solar Dynamics Observatory. Active regions are automatically detected and tracked during their passage over the solar disk. Each active region is enclosed in a box called a HARP (HMI Active Region Patch).

Acknowledgement [icon name=”bookmark” class=”” unprefixed_class=””] Swedish Institute of Space Physics (IRF) & (SSWC). Ref: The magnetograms are provided by NASA/SDO. The image above is created by JSOC/Stanford.


Sunspot

ASSA detected sunspot groups plot on SDO HMI magnetogram


Update Interval: 60 min.

Internal name: ASSA Detected Sunspot Groups Plot on SDO HMI Magnetogram
Cygnet Description: ASSA-detected sunspot groups plot displayed on SDO HMI Magnetogram.

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.

It is provided by the Korean Space Weather Center of National Radio Research Agency.

ASSA uses high resolution SDO HMI continuum and magnetogram data as inputs in 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.

The output results of ASSA are routinely checked and validated against NOAA’s daily SRS (Solar Region Summary) and UCOHO.

 


Corona

Solar corona (SDO/NASA)

Info: Solar flares are seen as bright regions in images observed by AIA onboard SDO. The intense electromagnetic radiation causes low frequency and HF communication problems.

Acknowledgement [icon name=”bookmark” class=”” unprefixed_class=””] Swedish Institute of Space Physics (IRF) & (SSWC). Ref: The SDO AIA data are produced by NASA/SDO


Corona

Solar corona (SOHO/NASA/ESA)

Info: Coronal mass ejections (CME).
CMEs are seen as large plasma clouds in coronagraph images observed by LASCO onboard SOHO.
The small white circle shows the size of the solar disk.

Acknowledgement [icon name=”bookmark” class=”” unprefixed_class=””] Swedish Institute of Space Physics (IRF) & (SSWC). Ref: The solar coronal images are produced by SOHO.


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