ASSA GUI User Manual
Contents
1. Values are used as of Apr 2013 20 5 Filament Detection To be updated later 5 1 GUI Interface To be updated later Description on GUI of filament detection If you select Filament Detection at Task Tab GUI for filament detection becomes active which looks like the following figure In the Filament Detection tab you can just view the latest image of filament detection result by pressing Show Latest Result button as of now in the current version The full functionalities of processing the appropriate data for filament detection wil be supported in the later version of ASSA GUI The contents of this section will also be updated then i NATIONAL RADIO RRAS ne SPACE ENVIRONMENT EAS ORATORY Filament Detection varal Main Display Window 5 2 Getting Raw Data To be updated later Description on Downloading Raw data 5 3 Data Processing To be updated later 21 Description on data processing 5 4 Result To be updated later Description on result of filament detection The latest result of filament detection is displayed by pressing Show Latest Result button as seen in the following figure This is the same image produced by ASSA system of RRA and being provided in ASSA web page the URL of which is as follows http www spaceweather go kr models assa NL Ass nn wr se enanala ole aerel Korel Detected Filaments i RRAS displayed on Udaiptir F alpha at 22. classification can also be browsed in a simple GUI by pressing Show Classification Details button Especially this interface has tab sections for each sunspot group showing the detailed 10 description on how the classification result was derived Each tab also shows the individual view of the corresponding sunspot group The following three figures show the examples of these two interfaces for inspecting the classification result more efficienly X Sunspot Classification Result ooo ooo IN Sunspot Classification Details Ooo X Sunspot Classification Details Physical parameters As described in the earlier section there are many parameters derived in the course of classification process in order to make decision in each step Each parameter has its default value which is used to produce the public version of figures for classification result which are currently updated at the ASSA website of RRA These parameters are summarized at the following table 11 Key Parameters for Sunspot Classification Parameter Value Unit factor of standard deviation to be subtracted from mean intensity to 6 0 None determine threshold intensity for sunspot detection factor of standard deviation to be applied to standard deviation based region growing 1S dana maximum separation between two sunspots to be considered to belong to the same spot group 6 0 Deore maximum separation
3. 1504 284 27 1020 40 i o 0 00 15 2 0 DAC 70 112 18 2 8 5 3 a ae 0 02 69 233 2 DAI 464 485 50 1 391 419 70 6 58 7 L 0 01 65 14 1 DAO 2069 845 102 2 1775 784 124 4 2 2 o 0 00 5 6 o DHC 52 3 o o o o 2 2 0 00 66 37 DHI d 6 8 u 4 1 8 8 ie L 0 00 7 9 o DHO 5n 2 t 46 26 1 1 u e o 0 01 37 9 1 DKC 100 200 43 7 57 93 35 5 mw 1 0 09 83 44 8 DKI 179 225 3 5 223 288 69 6 amp 6 a6 L 0 03 72 26 3 DKO 186 118 28 7 217 178 55 5 m 2 0 03 52 20 3 DRC 1 0 o o e o 0 00 8 o DRI ua i 2 7 7T 2 3 0 01 95 11 1 DRO 13 27 5 63 2 3 6 6 o 0 00 16 4 o psc to L t o o o o 5 2 6 0 07 31 20 7 DSI 108 72 6 33 34 6 31 1 82 0 11 0 00 56 10 0 D50 1695 423 53 1 546 1988 26 1 51 6 0 29 0 05 0 00 235 5 EAC 75 116 1 3 3 5 1 8 6 3 1 570 19 0 06 73717 6 EAI 454 561 77 4 295 370 83 2 48 1 1 24 0 25 0 01 n2 1 EAO 599 374 66 2 459 267 6 8 10 4 0 61 8 13 0 01 46 12 1 EHC 4 10 8 o 2 9 8 3 70 0 80 0 00 98 55 EHI 30 54 8 OO 15 2 6 28 4 1 67 0 47 0 04 81 37 4 EHO 31 29 2 6 42 31 6 6 6 0 79 0 13 0 00 55 12 0 EKC 231 567 114 18 103 278 132 17 149 21 2 56 0 99 0 14 92 63 13 EKI 324 455 71 10 423 73 13 23 103 11 1 56 0 42 0 05 73 34 5 EKO 155 133 26 1 185 173 35 3 20 1 0 90 0 21 0 01 68 19 1 ERO 5 2 12 o o o 0 40 0 20 0 00 33 18 ESC 8 8 2 o o o o 8 1 00 6 25 0 00 63 22 0 ESI 7 6 7 B 18 39 1 8 22 2 1 46 0 18 0 01 7 1 ESO 260 3 68 9 37 6 8 14 6 37 8 86 0 00 3 6 o FAC 31 56 9 o o o 1 81 0 29 0 00
4. Probability Description on flare probability calculation The C M X flare probabilities denoted on the resultant image are based on the result of 12 statistical analysis of solar region and flare data for a period of 1996 2011 which was performed by KSWC Korea Space Weather Center For this analysis past archive of GOES X ray flare data and Mcintosh class data was used to calculate average flare rate for each Mcintosh class This result was then used to determine Poisson flare probabilities for each flare class The analysis method presented in Bloomfield et al 2012 was adopted for this work The entire list of the result is shown in the following figure MeTontosh blReaions SWPC Kildahl Combined Poisson Region 1996 2011 1988 1996 1969 1976 Flare Rate Flare Prob Classes OnDisk C M X OnDisk C M X OnDisk C M X C M CRx AXX 2271 65 5 1 2748 82 10 2517 3 3 6 0 00 R A amp BXI U a E o o 2 o o 0 00 o 6 o 8x0 2736 155 8 OO 3342 217 18 1 1906 a a2 0 00 6 1 0 CAI 7a 2 s 27 14 6 8 19 o o 0 00 40 12 0 CA0 1236 273 24 1455 3651 38 2 i 1 o 0 00 2 3 6 CHI 3 ee 2 2 es 6 o 0 00 38 16 0 CHO gi 31 5 6 a8 2 2 1 8 2 0 01 2 5 1 CKC 1 6 8 o o e o 0 00 e o o CKI 8 4 2 7 4 6 6 2 0 04 54 23 4 cko 139 66 13 3 135 59 1 8 B 2 e 0 02 36 11 2 CRI 4 4 o 6 2 7 o 0 00 39 4 o CRO 754 97 B3 o 745 102 3 2 2 0 00 3 2 0 CSI 9 2 14 8 2 1 2 o 0 01 Dop a cso 2381 335 39
5. The classification algorithms required for this analysis are developed according to the descriptions on sunspot classification presented by SIDC Solar Influences Data Analysis Center which is available on the following link http sidc oma be educational classification php 3 2 Getting Raw Data Date should be specified at the interface for date selection Year month day hour can be selected for the desired UT date Any past date may also be selected as far as it can be selected from the pull down menus Select the date and time in GUI as the following figure If you click Current Date button date and time will be automatically set to latest available date and time Date UT Select Year 2013 Select Month a Select Day o Select Hour CEI Current Date Load Data Then click Load Data button ASSA program automatically checks the sub directory called data to find out whether the appropriate files already exist For sunspot classification ASSA mainly uses SDO HMI solar continuum image flattened and magnetogram image named as e YYYY MM DD _ hh mm ss _Ic_flat_1k jpg continuum image e YYYY MM DD _ hh mm ss _M_1k jpg magnetogram image Additionally SRS Solar Region Summary data issued daily by NOAA is also required But in case the SRS data for the selected date is not available yet the whole process continues without it If there are no appropriate files in data directory ASSA wi
6. between sunspots to determine unipolar or 30 Degree bipolar i factor of group width to determine threshold of distance between 05 None spots with penumbra x ratio penumbral area entire spot area to determine threshold of 02 Riese maturity of penumbra p R 25 if spot area gt 100 threshold of asymmetry of outline ellipse of spot S None threshold of north south diameter of spot 2 5 Degree threshold of ratio sum of spot areas entire group area to 04 pbn determine compactness i threshold of ratio plus polarity minus polarity to determine alpha eea 0 2 5 0 None threshold of number of effective neutral lines separating opposite 2 Kate polarity to determine beta or beta gamma Yalues are used as of Apr 2013 It should be noted that some of these parameters are adjustable in ASSA GUI application By pressing Show Config button located at the right bottom side of ASSA GUI users can change the value of each parameter on the pop up window which looks like the following figure Although there are only a few adjustable parameters yet in the version 1 0 more parameters are to be added in the upcoming version in near future Configuration for Sunspot Classification 1 draw coordinate grid on solar disk Ozno 1zyes I 6 0 factor of stddev to determine threshold intensiy 6 maximum separation between two spots to be considered to belong to the same group angle distance in deg Save Changes Exit 3 5 Flare
7. in some steps Each parameter has its default value which is used to produce the public version of figures for classification result which are currently updated at the ASSA website of RRA These parameters are summarized at the following table 24 Key Parameters for Filament Detection Parameter Value Unit factor of median intensity of solar disk to determine candidates for 0 82 None filament factor of median intensity of solar disk to determine candidates for 0 65 None sunspot factor of standard deviation to be applied to standard deviation 20 Bs based region growing j ERZE structuring elements for detection of filament like elongated feature FT T N None maximum separation between two fragments to be considered to 40 Pixel belong to the same filament Values are used as of Apr 2013 e References 1 Bloomfield D S Higgins P A McAteer R T J Gallagher P T ApJL 747 L41 2012 2 Colak T and Qahwaji R Solar Physics 248 277 2007 3 Krista L D and Gallagher P T Solar Physics 256 87 2009 4 Shih F Y and Kowalsky A J Solar Physics 218 99 2003 e Acknowledgement License 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 Contact Address 198
8. ten E wa es eno ke dit te a ee te yet EG Eile Polarity Distribution of the detected CHs ec tees EES ape coi cs oe os ice Mist sia TA CE SE ee tet 2a Distribution of Field Strengths RBE ser SBE RP es KE HE 9 F PERRA e00 Skewness i 1 40 Vien fears Wie L J ga L J Fe heath of wolar ck a woz SLS Eia E ZE 9 SSR U C0 al We Se Be L 4 S Be ag Gris eerie e F 4 Vie Scar Bais C Ve GS G Bacall 7 az SL EST aW L 4 ee Grae Eat L d ies Ste BLA HD R L J fer Shs ERE wan sear L 200 L ma L 4 Foe seo ele sk 105 Vee ile sees L 4 Wee Sa these Vii Socal ue Yas Sis ute io Sen tain Yso 1000 500 0 500 1000 1500 es Si 2 Field Strength G A 1 Clase Physical parameters As described in the earlier section there are many parameters derived in the course of coronal hole detection in order to make crucial decision in some steps Each parameter has its default value which is used to produce the public version of figures for classification result which are currently updated at the ASSA website of RRA These parameters are summarized at the following table Key Parameters for Coronal Hole Detection Parameter Value Unit factor of median intensity of solar disk to determine candidates for 0 45 wins coronal hole S lower limit of absoulte skewness of magnetic polarity distribution 0 6 None inside coronal hole area Pi lower limit of pixel area to be regarded as a coronal hole 2000 None
9. 015 Apr 12 0900 UTC 7 L SPACE ENVIRONMENT Lasar og rand Process aie her She Latet Rul Looney Filament detection requires ground H alpha image There s no H alpha images not only routinely observed by satellite but also being provided to the public in realtime GONG H alpha archive provides near realtime H alpha data observed at some representative ground solar observatories The available observing hour differs from observatory to observatory In ASSA system H alpha images from Big Bear Solar Observatory and Udaipur Solar Observatory are used because their entirely different time coverage in UT as follows makes it possible to cover 22 as many hours as possible 1 Udaipur 04 12 UT 2 Big Bear 16 24 UT The detailed work flow of filament detection in ASSA is shown in the following figure It should be noted that morphology opening plays a very important role in discriminating features of elongated shape typical of filaments For this purpose structuring elements of elongated shape with various direction angles are used for morphological opening Shih and Kowalsky 2003 As the figure shows many kinds of quantitative parameters are estimated to be used for decision The key parameters will be summarized at the following section 23 H alpha Image As described in the earlier section there are many parameters derived in the course of filament detection in order to make crucial decision
10. 3A Image SDO HMI Magnetogram Image Output files The latest output files generated after all processes are finished are automatically stored in a directory called gui_figures ASSA Output image is saved as C_Hole png Output text data is saved as ASSA_Hole txt which has the text resuts such as number of coronal holes serial number area location of vertices etc These output files are also stored in directories called gui_figures ASSA YYYY MM DD which are named according to the date The other output files generated from previous job for other date are also stored in this way so that you can find any previous output results once you ve worked Just keep in mind that there s no buttons for saving the results as all the output files are always saved in the designated directory Additional interfaces for browsing the detection results The text results described in ASSA_Hole txt can be browsed in a simple text window by pressing Show Text Result button The distribution of magnetic polarity inside each coronal hole can also be browsed in a simple GUI by pressing Show Polarity Distribution button Especially this interface has tab sections for each coronal hole showing each distribution plot The following two figures show the examples of these two interfaces for inspecting the detection 19 result more efficienly ian we Mise ar neta aa m Teed om sa ih 18
11. 6 Gwideok ro Hallim eup Jeju si Jeju do 695 922 Korea Phone 82 64 797 7031 Email spaceweather msip go kr feedback site http www spaceweather go kr assa 25 26
12. 84 25 0 FAI 142 237 3 91 106 35 3 8 1 46 0 32 0 01 7 28 1 FAO 108 7 2 2 73 63 16 0 81 0 22 0 01 56 19 1 FHC 10 3 1 6 o o o 4 2 20 1 80 0 00 89 63 6 FHI 10 24 5 o 1 7 9 6 15 1 88 0 76 0 00 85 53 0 FHO 2 12 2 s 5s 4 0 58 0 08 0 00 a 7 o FKC 223 614 186 32 93 233 146 24 39 13 2 67 1 08 0 20 93 66 18 FRI 184 388 80 9 235 517 161 17 106 17 2 16 0 74 0 09 89 53 9 FKO 69 68 10 6 97 165 29 1 6 1 43 0 24 0 01 76 22 1 FRO 1 o o o 0 00 0 00 0 00 o o o FSC 3 3 o o o 1 00 0 80 0 00 63 8 o FSI 2 3 3 6 6 2 15 1 71 0 53 0 00 82 41 o FSO 5428 7 4 9 3 8 6 1 0 56 0 20 0 01 43 18 1 HAX 851 78 7 598 49 13 o 14 0 090 030 009 8 3 0 HHX 103 17 1 R Z t 6 16 2 0 09 0 06 0 01 9 6 1 HKX 101 15 6 1 49 11 2 6 7 018 0 01 E a HRX 47 14 o o 336 2 2 1 8 211 7 1 0 05 0 01 0 00 5 1 0 HSX 3006 145 22 2 1968 94 21 0 1963 99 6 0 05 0 02 0 00 T HXX 1 o o o 8 0 00 0 20 0 00 e o o On the right bottom section of the resultant figures flare probabilities for C M X class is written with black colored letters Actually the probability value for each flare class is a representative value for all sunspot groups on the entire solar disk This probability for each flare class is calculated according to the following formula 13 Prob_total 1 1 P1 1 P2 1 P3 1 Pn Here n is the number of sunspot groups on the entire solar disk And each P values are the Pois
13. ASSA GUI User Manual Version 1 07 Last Updated 2013 7 11 1 Introduction ASSA is an abbreviation of Automatic Solar Synoptic Analyzer which is a name of the software system developed by the Korean Space Weather Center of the Radio Research Agency and SELab Inc in Korea ASSA consists of the following three categories 1 sunspot group identification and classification 2 coronal hole detection 3 filament detection ann Siasau cs Sunspot Group Detection amp Classification For each category ASSA receives necessary solar raw images and processes them in a designated procedure to yield resultant output files The whole procedure is performed every hour and the results are available on following website http www spaceweather go kr models assa ASSA GUI is a standalone program which enables users to emulate the whole procedures of 1 ASSA in their personal computers It is developed with IDL and wrapped up as a distributable file package so that every users can use it even if they don t have IDL installed on their computer With this program users can fully experience the detailed procedures of ASSA It features algorithms for data receiving image processing generating output results etc The current version 1 0 will be continuously updated based on feedbacks from users via this website 2 Installation ASSA GUI is currently available on Windows and Mac OS X Users can download the program pack
14. age on the following link according to each OS Windows http www spweather com lee ASSA ASSA_WIN32 zip Mac OS X http www spweather com lee ASSA ASSA_MAC64 zip Download the zip file and extract it anywhere you want on your hard drive Inside the extracted folder just double click a file named ASSA_MAC64 app on Mac OS X or ASSA_WIN32 exe on Windows If you already have IDL 8 x version on your PC the main GUI will appear If you don t have any IDL installed on your PC ASSA GUI program will be runned under IDL virtual machine environment thus two splash pop ups will appear as followings Z IDL Virtual Machine Application IDL Discover What s In Your Data lx HL 1000 10101010 j 010101 ox 10101 1010 740 ID Virtual Machine Distribution Platform To Run IDL Applications Just press buttons to continue and the main GUI will appear If you can see the main GUI which looks like the following figure you re ready and set 200 Nassa cur T NATIONAL RADIO PP nea SPACE ENVIRONMENT LABORATORY Sunspot Group Detection amp Classification Main Disply Window 3 Sunspot Classification amp Flare Probability 3 1 GUI Interface Description on GUI of sunspot classification In the Sunspot Classification tab you can identify sunspot group and obtain McIntosh and Mt Wilson magnetic classification results by processing SDO HMI continuum and magnetogram images
15. aily by NOAA is also required But in case the UCOHO data for the selected date is not available yet the whole process continues without it If there are no appropriate files in data directory ASSA will show a pop up window as follows Warning No data found Download from SDO data archive 0K Cancel Then press OK ASSA will connect to SDO FTP archive and download the files which are saved in ASSA data diectory data If you already have such files in your local disk and these files are named appropriately just copy them to ASSA data directory It also works When downloading SDO files is completed ASSA will show the appropriate AIA 193 and magnetogram images on the main display window as shown in the following figure You can switch to AIA 193 image or magnetogram image by clicking AIA 193 and Magnetogram tabs of Image Tab located at upper right side of Main Display Window 15 4 3 Data Processing After the appropriate data files are successfully downloaded and displayed you may choose either to process all steps one by one by pressing each button or to process all steps at once automatically in order in a pop up window which looks as follows Choose an option and press Continue button Notification Do you want to process step by step Or process all steps at once If you choose to process all steps at once buttons for each process remain inactive A Step By Step w A
16. ed If you choose to process all steps one by one Step 1 button for Continuum and Magnetogram tab becomes active By pressing Step 1 button the first procedure for data processing is performed After it s done the button for the next procedure Step 2 becomes active and so on The remaining buttons become active one by one in order according to the designated order of process which intuitively indicate what to do next for users Therefore users can recognize what is done for each process every step of the way For every step the display window shows the image resulting from that stage of process For example the 5 following figure shows the status when Step 6 button on Continuum tab is pressed and the corresponding process is done As can be seen the resultant image from Step 6 is displayed and Step 7 button becomes active It doesn t matter Step 1 button on which tab is first pressed In any way all Step buttons on both tabs will be highlighted in order ann Sassa cut a NT E l Sunspot Group Detection amp Classification bes ap var vear a03 a Classification After all procedures for continuum and magnetogram images are finished Do Sunspot Classification button becomes active Pressing this button invokes the procedure for estimation of Mcintosh and Mt Wilson magnetic class for each identified sunspot group This procedure may
17. ll Steps At Once Continue If you choose to process all steps at once automatically in order you have only to wait for all processes to be completed If you choose to process all steps one by one Step 1 button for AIA 193 and Magnetogram tab becomes active By pressing Step 1 button the first procedure for data processing is performed After it s done the button for the next procedure Step 2 becomes active and so on The remaining buttons become active according to the designated order of process which intuitively indicate what to do next for users For every step the display window shows the image resulting from that stage of process Therefore users can recognize what is done for each process every step of the way For every step the display window shows the image resulting from that stage of process For example the following figure shows the status when Step 2 button on AIA 193 tab is pressed and the corresponding process is done As can be seen the resultant image from Step 2 is displayed and Step 3 button becomes active It doesn t matter Step 1 button on which tab is first pressed In any way all Step buttons on both tabs will be highlighted in order 16 soo A assa cu 4 4 Result Description on result of corona hole detection After all necessary steps are completed the final result is displayed by pressing Show Final Result button as see
18. ll show a pop up window as follows Warning No data found Download from SDO data archive Ok Cancel Then press OK ASSA will connect to SDO FTP archive and download the files which are saved in ASSA data diectory data If you already have such files in your local disk and these files are named appropriately just copy them to ASSA data directory It also works When downloading SDO files is completed ASSA will show the appropriate continuum and magnetogram images on the main display window as shown in the following figure You can switch to continuum image or magnetogram image by clicking Continuum and Magnetogram tabs of Image Tab located at upper right side of Main Display Window 3 3 Data Processing Processing continuum and magnetogram images After the appropriate data files are successfully downloaded and displayed you may choose either to process all steps one by one by pressing each button or to process all steps at once automatically in order in a pop up window which looks as follows Choose an option and press Continue button Notification To you want to process step by step Or process all steps at once If you choose to process all steps at once buttons for each process remain inactive Step By Step All Steps At Once Continue If you choose to process all steps at once automatically in order you have only to wait for all processes to be complet
19. m R e Ke Ob st Let at ena Haste 1997 Alpha 0002 Alpha 2 Shi Tee Rl tou aian ai P I S SRS Issue Date 2013 Apr 03 0030 UTC Wolf Number 80 Output files The latest output files generated after all processes are finished are automatically stored in a directory called gui_figures ASSA Output images are saved as Spot_Mci png and Spot_Mag png for McIntosh classification result and Mt Wilson magnetic classification result respectively Output text data are saved as ASSA_Spot txt and ASSA_Spot_class txt ASSA_Spot txt has the text resuts such as number of spots location area class letter etc ASSA_Spot_class txt more detailed informations of the parameters used for classification These output files are also stored in directories called gui_figures ASSA YYYY MM DD which are named according to the date The other output files generated from previous job for other date are also stored in this way so that you can find any previous output results once you ve worked Just keep in mind that there s no buttons for saving the results as all the output files are always saved in the designated directory Additional interfaces for browsing the classification results The text results described in ASSA_Spot txt can be browsed in a simple text window by pressing Show Text Result button The detailed information of parameters estimated for
20. n in the following figure The polygons with red solid line correspond to the detected coronal holes by ASSA whereas the polygons with blue solid line correspond to the coronal hole reported by UCOHO data issued for the same day by SWPC UCOHO results are shown just for comparison 17 2 0 9 A R GIN a rat Hao ro ale Bin Flew S Detected Coronal Holes BI RRA SN based I FF SPACE ENVIRONMENT D LAG ORATORY Coronal Hole Detection tse it Select Year aois a Selec Herth N Select a 67 ie br 8 ET ESE ve 155 tater rere 3 ane Sp 1 Bld taking Sten 2 2 0 Semte Step 5 t teeta Cs Step d Tetersine CH ra hou Toe Roe Siri Werte a rue N ane oe deanna compared with UCOHO data issued at 2013 Apr 06 13 13 00 UTC The detailed work flow of coronal hole detection in ASSA is shown in the following figure It should be noted that the distribution of magnetic polarity inside each candidate area ofcoronal hole is examined This is based on the final decision method of differentiating coronal holes from filaments described in Krista and Gallagher 2009 If the skewness of distribution is sufficiently far from zero the corresponding area can be regarded as a coronal hole As the work flow in the following figure shows many kinds of quantitative parameters are estimated to be used for decision The key parameters will be summarized at the following section 18 SDO AIA 19
21. oth classification process in ASSA is shown in the following figure As the figure shows many kinds of quantitative parameters are estimated to be used for class decision The key parameters will be summarized at the following section Mcintosh Z of Zpe Mcintosh p of Zpe Mcintosh of Zpe Wilson Magnetic Class ans of sunspot group sel TU penumbra shape measure asymmetry The classification results are overlayed on the final resultant figures As can be seen in the following figure the McIntosh class Zpc estimated for each sunspot group is written on continuum image with brown colored letters along with the group number The same kind of information from SRS Solar Region Summary issued by NOAA on the same day is also written with green colored letters for comparison The issue date of SRS used for this figure is written at the bottom with green colored letters It should be kept in mind that SRS is issued once in a day for 00 30 UT The date of continuum image used for this analysis is also written at the top with violet colored letters On the upper left side of the figure the flare probabilities for C M X class are written with black colored letters On the right bottom side of the figure the Wolf number is also written with black colored letters The following formula is used to calculate Wolf number WN k 10g s s n
22. son probability from the above table 4 Corona Hole Detection 4 1 GUI Interface If you select Coronal Hole Detection at Task Tab GUI for coronal hole detection becomes active which looks like the following figure In the Coronal Hole Detection tab you can identify coronal holes by processing SDO AIA 193A and HMI magnetogram images aoo S assa cut IT TASK lab Sunspot Group Detection amp Classification Main Disply Window Status 4 2 Getting Raw Data Date should be specified at the interface for date selection Year month day hour can be selected for the desired UT date Any past date may also be selected as far as it can be selected 14 from the pull down menus Select the date and time in GUI as the following figure If you click Current Date button date and time will be automatically set to latest available date and time Date UT Select Year 2013 Select Honth 04 Select Day 02 Select Hour 08 Current Date Load Data Then click Load Data button ASSA program automatically checks the sub directory called data to find out whether the appropriate files already exist For sunspot classification ASSA mainly uses SDO HMI solar continuum image flattened and magnetogram image named as e YYYYL MM _ DD _ hh _ mm _ ss _84__SDO_AIA_193 jp2 AIA 193 image e YYYY MM DD _ hh mm ss _M_1k jpg magnetogram image Additionally UCOHO data issued d
23. take some time from a few tens of seconds to a few minutes depending on CPU performance After the classification procedure is completed the classification results are shown overlapped on each image as follows These final resultant images looks the same as those images available on ASSA web page of RRA Detected Sunspot Groupe Detected Sunspot Groups j atp ar at 2018 Aer 09 0109 UTC Sparar H nes SN nec 100 S BE a as 3 4 Result Description on the results of sunspot classification In ASSA GUI sunspot classification consists of Mcintosh classification and Mt Wilson magnetic classification The algorithms developed for Mcintosh classification is applied to each sunspot group identified on continuum image in order to determine Zpc class of each group The algorithms developed for Mt Wilson magnetic classification is applied to each sunspot group superposed on magnetogram image in order to determine magnetic class of each group The basic concept of classifications described by SIDC Solar Influences Data Analysis Center in the following link has been mainly referred in order to develop algorithms for classification process in ASSA http sidc oma be educational classification php The pioneering work of digital implementation of sunspot classification by Colak and Qahwaji 2007 was also referred in developing the classification algorithms for this program The detailed work flow of b
24. umber of individual sunspots g number of sunspot groups k correction factor assumed to be 1 0 The C M X flare probabilities are based on the result of statistical analysis of solar region and flare data for a period of 1996 2011 which was performed by KSWC Korea Space Weather Center More details are described in section 3 5 geg N ASSA GUI SRS Issue Date 2013 Apr 03 0030 UTC Wolf Number 80 The Mt Wilson magnetic class estimated for each sunspot group is written on magnetogram image with brown colored letters along with the group number as seen in the following figure The same kind of information from SRS Solar Region Summary issued by NOAA on the same day is also written with blue colored letters for comparison The issue date of SRS used for this figure is written at the bottom with green colored letters The date of magnetogram image used for this analysis is also written at the top with violet colored letters On the upper left side of the figure the flare probabilities for C M X class are written with black colored letters On the right bottom side of the figure the Wolf number is also written with black colored letters cr tert Hole oree Dt en Detected Sunspot Groups i RRA ence displayed on SDO HMI Magnetogram at 2018 Apr 03 0100 UTC wo g E C Flare 02 m gt ans M Flare 39 Bi X Flare 1 Sunspot Group Detection amp Classification Be OW Slat tor ml iet ett Simt
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