Preparation for the analysis offilament eruptions
S.UeNo & K. Otsuji(Hida Observatory
Kyoto University)①

Installation of IDL in “C:¥Program Files¥”②Installation of Solar SoftWare (SSW) in “C:¥” fromhttp://www.lmsal.com/solarsoft/exe_client/ssw_install170511_195238.ZIP③

Copy of IDL programs for “Cloud Model Fitting” (calculation ofphysical values of filaments) under user’s folder. (1)④Copy of IDL programs for “Cloud Model Fitting” (calculation ofphysical values of filaments) under user’s folder. (2)⑤

Download of solar image data (SMART H-alpha data) under your data
folder as follows from the web-site of Kyoto University (=> see next page).

⑥

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/← Please click “T1 Data Archive”⑦

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/← If you want to download the data on
2011/09/08, please click “Before 2016 Apr”⑧

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/← If you want to download the data on
2011/09/08, please click “2011-Sep”.

⑨

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/← If you want to download thedata on 2011/09/08,
please click this image.

⑩

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/

Before the download, you can check moviesof this day by clicking “Javascript Movie”.
Please click “Download FITS files” fordownload of data files.

⑪

Download site of SMART solar image data:
http://www.hida.kyoto-u.ac.jp/SMART/(2) Select “checked files” andPush the “download” button.

(1) Please check “File No.”sthat you want.

⑫

Hida observatory SMART T1
Cloud model application method
K. Otsuji
Hida Observatory, Kyoto University
2017/05/22⑬

About this manual• To apply Beckers’ cloud model (Beckers 1964) toH alpha multi-wavelengths observation by SMART
in Hida observatory.
• Using IDL code, fitting the contrast profile of“cloud” on the observed data, derivation of cloudparameters (Source function, Optical depth,
Doppler width and Doppler shift).
• The local correlation tracking (LCT) method isapplied to derive transversal motion on the image
plane.
⑭

IDL programs•

prep.pro•cont.pro•param.pro•trans.pro– Specify data directory– Create calibration files (dark and flat frames)– Select dataset and output the list of files– Define the field of view of clipped data
– Calibration and contrast calculation– Output clipped fits files and gif images– Apply cloud model to the contrast datasets– Output parameters fits files and gif images– Calculate the 2nd level Hydrogen column density and derive the transversal
velocity field using local correlation tracing– Output the parameters fits files and gif images⑮

Startup• Click the “SSWIDL” iconon the desktop andstart the IDL with Solar
SoftWare (SSW)⑯

prep.pro (1)Open prep.pro and “コンパイル(compile)” -> “実行(execute)”⑰

prep.pro (2)• Data directory selecting
dialog open
• Select the directory forprocess• In this demonstration,please select“C:¥data¥SMART¥pub¥
2011¥09¥08¥T1¥”• Click “Accept”

directory selecting dialog⑱

prep.pro (3)• Calibration files are output in theIDLWorkspace¥T1_cloudmodel¥20110908¥calib

Dark and flat frame images⑲

prep.pro (4)• File selection dialog open
• Click the file name and toggle include/exclude
from the file list
• In this demonstration, all files are included• Click “Done”

File selection dialog⑳

prep.pro (5)Output IDLWorkspace¥T1_cloudmodel¥20110908¥fitslist.csv(21)

prep.pro (6)Output IDLWorkspace¥T1_cloudmodel¥20110908¥obstime.gif(22)cont.pro (1)Open cont.pro and “コンパイル(compile)” -> “実行(execute)”(23)

cont.pro (2)• Save directory selectingdialog open
• Select the directory forprocess• In this demonstration,please select“20110908¥”• Click “Accept”

directory selecting dialog(24)

cont.pro (3)• 9 Contrast images arecalculated• window open
• Click the image to set
the FOV of clipped data(25)

cont.pro (4)• displaying the selected
full FOV image• Using mouse to
move/enlarge/shrink
the FOV of clipping area.
– left click + drag: move– middle click + drag:enlarge/shrink– right click: done

(26)cont.pro (5)Output contrast image gifs in IDLWorkspace¥T1_cloudmodel¥20110908¥gif¥cont¥
Fits files are output as 20110908¥fits¥cont_*.fits(27)

param.pro (1)Open param.pro and “コンパイル(compile)” -> “実行(execute)”(28)

param.pro (2)• Save directory selecting
dialog open
• Select the directory forprocess• In this demonstration,please select“20110908¥”• Click “Accept”

directory selecting dialog(29)

param.pro (3)Cloud model fitting progress is shown
Doppler shift map is displayed in the right panel(30)

param.pro (4)Output 4 parameter image gifs in
IDLWorkspace¥T1_cloudmodel¥20110908¥gif¥{source,optical,width,doppler}¥
Fits files are output as 20110908¥fits¥param_*.fits(31)

trans.pro (1)Open trans.pro and “コンパイル(compile)” -> “実行(execute)”(32)

trans.pro (2)• Save directory selecting
dialog open
• Select the directory forprocess• In this demonstration,please select“20110908¥”• Click “Accept”

directory selecting dialog(33)

trans.pro (3)Output transversal (apparent) velocity image gifs in
IDLWorkspace¥T1_cloudmodel¥20110908¥gif¥trans¥
Fits files are output as 20110908¥fits¥trans_*.fits(34)

Summary• Using this IDL codes, one can easily derive thephysical parameters such as the 3 dimensional
velocity field and the density of filaments.
• comments or questions– to otsuji@kwasan.kyoto-u.ac.jp(35)