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lasco_mk_html_help.pro
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Fri Jan 12 09:28:43 2007.
There are several "main" programs that may be useful to calculate the mass or electron density (columnar) in CMEs. The mass of a CME is computed from the excess brightness after having subtracted off the pre-event brightness. The technique is to recognize that a single electron at a certain point in the atmosphere will scatter a known amount of the solar disk intensity. Then by knowing the observed intensity, and by assuming that all of the mass is in a single volume element, we can compute the number of electrons. Then assuming charge neutrality, the mass can be computed. The various procedures that can be used to compute electron density or mass are: C3_CME: A function to calibrate C3 images and calculate the mass of a CME given the base and cme image. C3_CME_FRONT: A function to calibrate C3 images and to calculate the mass of the CME front. C3_MASSIMG: A function to calibrate C3 images and calculates the mass of a CME. The output is a file that is a mass (or electron density image). CME_MASSIMG2TOTAL: This function allows you to specify the area of features for which to calculate the mass of a CME from mass images. rah 3/26/99
NAME: C3_CME PURPOSE: This function calibrates C2 & C3 images and calculates the mass of a CME CATEGORY: CME CALLING SEQUENCE: Result = C3_CME,Bn,Fn INPUTS: Bn: String containing the filename of the base image Fn: String containing the filename of the CME image KEYWORD PARAMETERS: MINSCL: Set this keyword with the value to use for the minimum value in scaling the image. The default value is to use -1.e-11 msb MAXSCL: Set this keyword with the value to use for the maximum value in scaling the image. The default value is to use +1.e-11 msb SAVE: Set this keyword with the filename to save the mass information to OUTPUTS: This function returns the mass calculated for the ROI selected RESTRICTIONS: Only works for C3 EXTERNAL CALLS: DEFROI, C2_CALIBRATE, C3_CALIBRATE, LASCO_READFITS, CALC_CME_MASS PROCEDURE: The files for the base and CME images are read in and calibrated. The images are then adjusted to have the same area and summing. The images are differenced, displayed and then DEFROI is called to get the desired region of interest. CALC_CME_MASS is called to compute the CME mass. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the mass information in 'mass.lst': Mass = C3_CME ('320004.fts','320005.fts',save='mass.lst') MODIFICATION HISTORY: Written by: RA Howard, NRL, 5/19/97 MOdified: RAH 3/14/98, changed rebin of b to calb %W% %H% LASCO IDL LIBRARY
NAME: C3_CME_FRONT PURPOSE: This function calibrates C3 images and calculates the mass of a CME CATEGORY: CME CALLING SEQUENCE: Result = C3_CME_FRONT,Bn,Fn INPUTS: Bn: String containing the filename of the base image Fn: String containing the filename of the CME image KEYWORD PARAMETERS: MINSCL: Set this keyword with the value to use for the minimum value in scaling the image. The default value is to use -1.e-11 msb MAXSCL: Set this keyword with the value to use for the maximum value in scaling the image. The default value is to use +1.e-11 msb SAVE: Set this keyword with the filename to save the mass information to NEW: Set this keyword if the base image is new SECTOR: Set this keyword if the ROI is a sector, centered on the sun RADII: Set this keyword with a 2-element array of the inner and outer radii (in solar radii) for the sector ROI ANGLES: Set this keyword with a 2-element array of the left and right hand boundaries (viewed from sun-center) for the sector ROI OUTPUTS: This function returns the mass calculated for the ROI selected RESTRICTIONS: Only works for C3 EXTERNAL CALLS: DEFROI, C3_CALIBRATE, LASCO_READFITS, CALC_CME_MASS, ROI_SECTOR AWIN, AVERAGE PROCEDURE: The files for the base and CME images are read in and calibrated. The images are then adjusted to have the same area and summing. The images are differenced, displayed and then DEFROI is called to get the desired region of interest. CALC_CME_MASS is called to compute the CME mass. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the mass information in 'mass.lst': Mass = C3_CME_FRONT ('320004.fts','320005.fts',save='mass.lst') MODIFICATION HISTORY: Written by: RA Howard, NRL, 5/19/97 @(#)c3_cme_front.pro 1.2 10/03/99 LASCO IDL LIBRARY
NAME: C3_MASSIMG PURPOSE: This function calibrates C3 images and calculates the mass of a CME CATEGORY: CME CALLING SEQUENCE: Result = C3_MASSIMG(Bn,Fn) INPUTS: Bn: String containing the filename of the base image Fn: String containing the filename of the CME image KEYWORD PARAMETERS: SAVE: If set, appends the total mass into a file. If the keyword is a string, then the filename is the string otherwise the user is prompted for the file name. ONLY_NE:If set, then compute electron density rather than mass NEW: If set, then process the base image, even if it has been done OUTPUTS: This function returns an image of the calculated mass RESTRICTIONS: Only works for C3 EXTERNAL CALLS: C3_CALIBRATE, LASCO_READFITS, CALC_CME_MASS PROCEDURE: The files for the base and CME images are read in and calibrated. The images are then adjusted to have the same area and summing. The images are differenced. CALC_CME_MASS is called to compute the CME mass. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the total mass information in 'mass.lst': Massimg = C3_MASSIMG ('320004.fts','320005.fts',save='mass.lst') MODIFICATION HISTORY: Written by: RA Howard, NRL, 6/9/97 RAH 5/23/98, Make work and make similar to c3_cme_front @(#)c3_massimg.pro 1.4 10/03/99 LASCO IDL LIBRARY
NAME: CALC_CME_MASS PURPOSE: Computes the CME mass in an image given a box defining the area CATEGORY: CME CALLING SEQUENCE: Result = CALC_CME_MASS (Img, Hdr, Box) INPUTS: Img: The 2-D difference image containing the CME. The units are in mean solar brightness units Hdr: The lasco header structure of the image Box: An array containing the coordinates of the region of interest KEYWORD PARAMETERS: FNAME: If present, this string defines the name of a file to store the mass value in. The information will be appended to an existing file or will create a new file. The default is not to save the information. CONT: If set this parameter indicates that a continuing CME sequence is being computed and various parameters will be not be computed. The default is to compute the parameters. POS: If present, this allows the angle from the plane of the sky to be specified. The default is to set the angle to 20 degrees. ROI: If present, then box contains the ROI indices rather than coordinates ALL: If present, then the entire image is processed ONLY_NE:If present, electron density is returned, rather than mass MAXVAL: If present, the maximum value in the region is computed MEDVAL: If present, the median value in the region is computed PB: If present, the input image is a pB image OUTPUTS: This function returns the mass contained within the ROI box in grams. COMMON BLOCKS: CME_MASS,Dist,Angle,B,Conv Dist = Distance of pixel in solar radii from sun center Angle = Angle of pixel in degrees from solar north B = brightness array of one electron Conv = Conversion factor from MSB to grams This common block is used to store a previous computation of the distance matrix to save time. SIDE EFFECTS: None RESTRICTIONS: The coordinates of the sun center must be in the header. PROCEDURE: An array in which the elements are the distance of that pixel from sun center is computed. Then ELTHEORY is called to compute the brightness and polarization properties of a single electron. MODIFICATION HISTORY: Written by: R.A. Howard, NRL, 18 September 1996 RAH 22 Mar 1997, Added Keyword POS and corrected mass/e RAH 16 May 1997, Changed header from FITS to header structure RAH 19 Sep 1997, Added Keyword ONLY_NE, added function of date RAH 18 Apr 1999, Put Ne to mass conversion into separate routine RAH 28 Sep 1999, Put POS (Plane of sky) angle to 0 instead of 20 RAH 03 Oct 1999, Added capability for pB image @(#)calc_cme_mass.pro 1.9 10/03/99 :NRL Solar Physics
NAME: CME_MASS PURPOSE: This function calculates the mass of a CME from calibrated images CATEGORY: CME CALLING SEQUENCE: Result = CME_MASS(Bn,Fn) INPUTS: Bn: String containing the filename of the base image Fn: String containing the filename of the CME image KEYWORD PARAMETERS: MINSCL: Set this keyword with the value to use for the minimum value in scaling the image. The default value is to use -1.e-11 msb MAXSCL: Set this keyword with the value to use for the maximum value in scaling the image. The default value is to use +1.e-11 msb SAVE: Set this keyword with the filename to save the mass information to OUTPUTS: This function returns the mass calculated for the ROI selected RESTRICTIONS: Only works for C3 EXTERNAL CALLS: DEFROI, C3_CALIBRATE, LASCO_READFITS, CALC_CME_MASS PROCEDURE: The files for the base and CME images are read in and calibrated. The images are then adjusted to have the same area and summing. The images are differenced, displayed and then DEFROI is called to get the desired region of interest. CALC_CME_MASS is called to compute the CME mass. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the mass information in 'mass.lst': Mass = C3_CME ('320004.fts','320005.fts',save='mass.lst') MODIFICATION HISTORY: Written by: RA Howard, NRL, 5/19/97 MOdified: RAH 3/14/98, changed rebin of b to calb %W% %H% LASCO IDL LIBRARY
NAME: CME_MASSIMG2TOTAL PURPOSE: This function calculates the mass of a CME from mass images. CATEGORY: CME CALLING SEQUENCE: Result = CME_MASSIMG2TOTAL(Fn) INPUTS: Fn: String containing the filename of the CME mass image KEYWORD PARAMETERS: MINSCL: Set this keyword with the value to use for the minimum value in scaling the image. The default value is to use -1.e-11 msb MAXSCL: Set this keyword with the value to use for the maximum value in scaling the image. The default value is to use +1.e-11 msb SAVE: Set this keyword with the filename to save the mass information to SECTOR: Set this keyword if the ROI is a sector, centered on the sun The default is to draw the boundary of the CME using the cursor RADII: Set this keyword with a 2-element array of the inner and outer radii (in solar radii) for the sector ROI ANGLES: Set this keyword with a 2-element array of the left and right hand boundaries (viewed from sun-center) for the sector ROI OUTPUTS: This function returns the mass calculated for the ROI selected RESTRICTIONS: Only tested on C3, but should work for any telescope EXTERNAL CALLS: DEFROI, LASCO_READFITS, ROI_SECTOR, AWIN, AVERAGE, XLOADCT, RDPIX PROCEDURE: The files for the CME mass image is read in. The image is displayed and XLOADCT is called to permit the contrast to be adjusted. Then RDPIX is called to permit individual pixel values to be displayed. If neither SECTOR, RADII, nor ANGLES are set, then the ROI is selected using the cursor to draw the boundary by using DEFROI. If only SECTOR is set then the ROI is an annular sector whose vertex is the sun center and the radii and angles of the sector are determined interactively. If RADII is set then the radial values are set to the input and similarly if ANGLES is set. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the mass information in 'mass.lst': Mass = CME_MASSIMG2TOTAL ('320004.fts','320005.fts',save='mass.lst') To use an annular sector, with boundaries defined interactively: Mass = CME_MASSIMG2TOTAL ('320004.fts','320005.fts',save='mass.lst',/SECTOR) To use an annular sector, with angular boundaries pre-set : Mass = CME_MASSIMG2TOTAL ('320004.fts','320005.fts',save='mass.lst',/SECTOR,ANGLES=[250,280]) or, since the SECTOR keyword is not necessary: Mass = CME_MASSIMG2TOTAL ('320004.fts','320005.fts',save='mass.lst',ANGLES=[250,280]) MODIFICATION HISTORY: Written by: RA Howard, NRL, 5/19/97 Modified: RAH, NRL, 3/14/98, comments added @(#)cme_massimg2total.pro 1.2 10/03/99 LASCO IDL LIBRARY
NAME: CW_ZOOM1 (modified version of CW_ZOOM). PURPOSE: This compound widget displays two images: an original image in one window and a portion of the original image in another. The user may select the center of the zoom region, the zoom scale, the interpolation style, and the method of indicating the zoom center. CATEGORY: Compound widgets. CALLING SEQUENCE: Widget = CW_ZOOM1(Parent) INPUTS: Parent: The ID of the parent widget. KEYWORD PARAMETERS: FRAME: If set, a frame will be drawn around the widget. The default is FRAME=0 (no frame). MAX: The maximum zoom scale, which must be greater than or equal to 1. The default = 20. MIN: The minimum zoom scale, which must be greater than or equal to 1. The default = 1. RETAIN: Controls the setting for backing store for both windows. If backing store is provided, a window which was obscured will be redrawn when it becomes exposed. Set RETAIN=0 for no backing store. Set RETAIN=1 to "request backing store from server" (this is the default). Set RETAIN=2 for IDL to provide backing store. SAMPLE: Set to zero for bilinear interpolation, or to a non-zero value for nearest neighbor interpolation. Bilinear interpolation gives higher quality results, but requires more time. The default is SAMPLE=0 (bilinear interpolation). SCALE: The initial integer scale factor to use for the zoomed image. The default is SCALE=4. The scale must be greater than or equal to 1. TRACK: Set to zero if the zoom window should be updated only when the mouse button is pressed. Set to a non-zero value if the zoom window should be updated continuously as the cursor is moved across the original image. Note: On slow systems, /TRACK performance can be inadequate. The default is TRACK=0. UVALUE: The user value for the widget. XSIZE: The width of the window (in pixels) for the original image. The default is 500. YSIZE: The height of the window (in pixels) for the original image. The default is 500. X_SCROLL_SIZE: The width of the visible part of the original image. This may be smaller than the actual width controlled by the XSIZE keyword. The default is 0, for no scroll bar. Y_SCROLL_SIZE: The height of the visible part of the original image. This may be smaller than the actual height controlled by the YSIZE keyword. The default is 0, for no scroll bar. X_ZSIZE: The width of the window for the zoomed image. The default is 250. Y_ZSIZE: The height of the window for the zoomed image. The default is 250. OUTPUTS: The ID of the created widget is returned. SIDE EFFECTS: When the "Report Zoom to Parent" button is pressed, this widget will generate an event structure containing several data fields. x_zsize, y_zsize: size of the zoomed image x0, y0: lower left corner in original image x1, y1: upper right corner in original image This event is a report to the parent that allows retrieval of the zoomed image using WIDGET_CONTROL. Ed Esfandiari August 1998: Removed "Report Zoom to Parent" button by commenting it out. PROCEDURE: WIDGET_CONTROL, id, SET_VALUE=value can be used to change the original, unzoomed image displayed by the widget. The value may not be set until the widget has been realized. WIDGET_CONTROL, id, GET_VALUE=var can be used to obtain the current zoomed image displayed by the widget. MODIFICATION HISTORY: June 30, 1992, ACY 7 April 1993, AB, Removed state caching. 13 June, 1994, ACY, Save window and set to zoom prior to erase Add byte conversion in set_value 23 November, 1994, ACY, add code to handle cases in which the set_value image is larger or smaller than the original image. Also remove scaling on display operation (only scale the image when it is set.) 06 August 1998, Ed Esfandiari, removed "Report Zoom to Parent" button and added "Show Zoomed Area" button which draws a box on the region of the original image corresponding to the zoomed image. This box will be dragged if the "Track Cursor" is set. Also the coordinates of the lower-left and upper-right corners of the box are displayed. If "Show Zoomed Area" is not set, only the cursor location is displayed. Finally, I changed the name of this program to cw_zoom1.pro.
NAME: GET_CME_SUMMARY PURPOSE: This function defines the cme_summary data structure CATEGORY: CME CALLING SEQUENCE: GET_CME_SUMMARY OUTPUTS: This function returns an empty CME structure. COMMON BLOCKS: com_xplot_ht SIDE EFFECTS: Initiates the XMANAGER if it is not already running. RESTRICTIONS: MODIFICATION HISTORY: Written by: RA Howard, NRL 12 May 1997 @(#)get_cme_summary.pro 1.1 05/14/97 :NRL Solar Physics
NAME: MLO_MASSIMG PURPOSE: This function subracts the input calibrated images into a mass image CATEGORY: CME CALLING SEQUENCE: Result = MLO_MASSIMG(Bn,Fn) INPUTS: Bn: String containing the filename of the base image Fn: String containing the filename of the CME image KEYWORD PARAMETERS: ONLY_NE:If set, then compute electron density rather than mass NEW: If set, then process the base image, even if it has been done OUTPUTS: This function returns an image of the calculated mass RESTRICTIONS: Only works for calibrated images EXTERNAL CALLS: LASCO_READFITS, CALC_CME_MASS PROCEDURE: The files for the base and CME images are read in and calibrated. The images are then adjusted to have the same area and summing. The images are differenced. CALC_CME_MASS is called to compute the CME mass. EXAMPLE: To find the mass of a CME, where the base image is '320004.fts' and the CME image is in '320005.fts', and saving the total mass information in 'mass.lst': Massimg = MLO_MASSIMG ('320004.fts','320005.fts') MODIFICATION HISTORY: Written by: RA Howard, NRL, 8/28/98 from C3_MASSIMG RAH 5/23/98, Make work and make similar to c3_cme_front %W% %H% LASCO IDL LIBRARY
NAME: NE2MASS PURPOSE: This function converts electron density into mass CATEGORY: CME CALLING SEQUENCE: Result = NE2MASS (Num_el) INPUTS: Num_el: The number of electrons OUTPUTS: This function returns the mass corresponding to the electron density. PROCEDURE: MODIFICATION HISTORY: Written by: R.A. Howard, NRL, 18 September 1996 @(#)ne2mass.pro 1.1 04/18/99 :LASCO IDL LIBRARY
NAME: ROI_SECTOR PURPOSE: This function returns the 1D list of indices contained within the specified sector CATEGORY: CME CALLING SEQUENCE: Result = ROI_SECTOR (Hdr,R1,R2,T1,T2) INPUTS: Hdr: Image header (LASCO header structure) R1: Inner radius of the sector (in solar radii), from sun center R2: Outer radius of the sector (in solar radii), from sun center T1: Left hand boundary of the sector (in degrees) T2: Right hand boundary of the sector (in degrees) KEYWORD PARAMETERS: PIXEL: If set, the inner and outer radii are specified in pixels DRAW: If set, the perimeter of the sector is drawn on the image OUTPUTS: This function returns the indices of the pixels contained within the sector as an array of long integers. COMMON BLOCKS: None SIDE EFFECTS: None RESTRICTIONS: PROCEDURE: A sector is defined as the region bounded by two radial lines (from sun center) at two position angles and the annulus (centered on the sun) at two heights. The pixel coordinates of the inner and outer boundaries of the annulus are computed at one degree increments from one position angle to the next. Correction is made if the sector spans the North pole (where the position angle is 0/360). POLYFILLV is used to fill in the indices from the definition of the boundary. The image header is used in determining the sun center and the number of pixels per radius. CALLED ROUTINES: GET_SUN_CENTER, GET_SOLAR_RADIUS, POLYFILLV EXAMPLE: To obtain the indices of a sector from 5 to 10 solar radii and position angles 270 to 280. Note that the left hand boundary as viewed from the sun is 280 and the right hand boundary is 270. The outline of the sector is drawn on the display Result = ROI_SECTOR(hdr,5,10,280,270,/draw) MODIFICATION HISTORY: Written by: RA Howard, NRL, 2 December 1997 @(#)roi_sector.pro 1.1 03/14/98 LASCO IDL LIBRARY
NAME: XCME_MES PURPOSE: This procedure is used to display CME measurements CATEGORY: CME CALLING SEQUENCE: XCME_MES INPUTS: OPTIONAL INPUT PARAMETERS: Filename: If filename is present then it is used immediately OUTPUTS: OPTIONAL OUTPUT PARAMETERS: COMMON BLOCKS: com_xcme_mes SIDE EFFECTS: Initiates the XMANAGER if it is not already running. RESTRICTIONS: PROCEDURE: MODIFICATION HISTORY: Written by: RA Howard, NRL, 7 May 1997 @(#)xcme_mes.pro 1.2 03/03/98 :NRL Solar Physics
lasco_mk_html_help.pro
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Fri Jan 12 09:28:43 2007.