;OBS TAB (only there for integrated quantities, not Physical Diagnostics or Data) ; ; TAB HEADER: keyword LINE - ; Default PB if neither line nor ; instrument set; If instrument is set but not line there is a ; different default for each instrument. ; ; keyword INSTRUMENT - ; Default 'WL' (white light) ; for cases where neither line nor instrument is set ; ; keyword POS (on or off) forces a plane of sky calculation for observables ; so integration is only over one LOS pixel ; If LOSUSE (see below) set to XLOS it will be the X=0 plane of sky ; If LOSUSE set to TLOS it will be the Thomson Sphere ; ; Choice of radial filter ; ; keyword RFILTER (NO_FILTER, AIA_FILTER, NRGF_FILTER, QUARTERPOWER_FILTER,GAMMA_FILTER,RPOWER_FILTER) ; only AIA DATA allows choice of AIA_RFILTER ; NRGF by Fineschi (based on Morgan et al SP 2006) ; GAMMA is gamma corrected (by chosen dispgamma) with chosen exponent (dispexp) ; RPOWER_FILTER is intensity times plane of sky radial position raised to a chosen exponent (rpow) ; QUARTERPOWER is just intensity raised to the quarter-power ; -- all act to enhance structure at higher radii ; (NOTE that activating keyword "PLOTLOG" (under Plot tab) has a similar effect) ; WARNING! Units are not meaningful for filtered data, and color table ; label will included "FILTERED" to indicate this. ; ; If temperature-sensitive observable: ; ; keyword POP2ON (1 or 0) ; turns on and off population 2 - needs to be on ; for POP2COLDEN or POP2LOSEM (see Observables), and for POP2TREGIME button to appear ; Note, if the model does not have Pop2 capability, POP2ON ; will be set to zero, and with it POP2TREGIME ; ; keyword POP2TREGIME - temperature regime for a second population if defined, ; if set to 1, treats second population as coronal, and ; can have different POP2ABUNDANCE ; if set to 2, treats second population as chromospheric and applies ; Lyman absorption (POP2IONFRAC input) ; NOTE if calculating non-spectral observable (e.g. WL, EM...) there is ; no difference between POP2TREGIME=1 and 2 ; if set to 3, second population density is set to zero so does not contribute to los integrals ; if set to 0 (default), second population ignored (this will be forced ; for POP2ON=0, and vice verse). ; if model CAVMORPH, Pop2TRegime will be forced by parameter choice ; so can't be set by user and should not appear in widget ; ; if spectropolarimetric instrument (e.g. CoMP) have ; ; keyword ROTAZ ; option of changing reference frame ; this will affect Q, U, and Azimuth ; choices are radial (frame w.r.t. local vertical) ; N-S (frame w.r.t sun's rotation axis) ; E-W (frame w.r.t. equator ; ; ; if WL have option of turning on/off F corona ; ; keyword FCOR ; using Koutchmy-Lamy formula ; ; also if WL can change limb darkening coefficient to match whitelight center wavelength (see ; keyword ULIMB ; WL default 0.63, appropriate for centered on 520 nm ; See Altschuler & Perry 1972 p 415 ;If UV Spectropolarimeter can look at limb brightening ; keyword ULIMB ; default 0 -- no limb brightening ; changing to any nonzero number scales ; a polynomial fit to Withbroe 1970 Ne8 and O6 ; This modifies the CHROMORAD (see below) ; that can act both as a source of resonant scattering ; and on disk as additional emission contribution ; Other lines so far do not have keyword visible ; ; if RADIO or FARADAY have choice of frequency ; ; keyword FREQUENCY_MHz ; ; if RADIO have choice of whether to do gyroresonance (or just ; Bremstrahllung) ; ***NOTE -- no ray tracing is done in these calculations, ; ***** at low frequencies, refraction can be important so ; ***** this needs to be considered. ; keyword DOGYRO ; ; if EUV spectrogram instrument (EIS, CDS, IRIS, MYSPECT, IONDENS) have choice of frequency ; ; keyword WAVELENGTH_ANG (Angstroms) ; keyword WAVELENGTH2_ANG (Angstroms) -- only used for WL spectroscopy (WLRAT) ; ; and also ion number ; ; keyword NUMION (integer) ; (note element is assigned in Observables drop-down menu) ; ; SEESPEC TAB ; ; ONLY VISIBLE FOR EUV/XRAY IMAGERS AND SPECTROMETERS/SPECTROPOLARIMETERS ; ; keyword SEESPEC - used by widget to toggle visibility of other keywords ; default 1 (on) ; (note not all are necessarily displayed) ; ; keyword ABUNDANCE - default to 'sun_coronal_1992_feldman' ; ; keyword POP2ABUNDANCE - default to ABUNDANCE ; ; keyword CVERSION - Chianti version, default is most recent ; ; keyword LLIM - emissivity limit for which lines to include ; ; keyword LWIDTH - linewidth for spectograph instruments. ; ; FOR UVMODEL ; ; ONLY VISIBLE FOR UV SPECTROPOLARIMETERS ; ; keyword NANGLEINT -- how many steps to take in integrating ; over solid angle for incoming radiation ; ; keyword COLLKEY - whether to do collisions and scattering (1) ; or just scattering (0) ; or just collisions (-1) ; ; keyword ISOTROPIC - whether to do isotropic (1) or ; anisotropic (0) model (UVMODEL ONLY) ; If set, any ModSolStruct.AnIso will be ignored (see below) ; ; keyword WPAR_OPEN, WPAR_CLOSED -- multiplicative factors ; to establish W_PAR if not set in ModSolStruct ; factors multiplying W_MIN which depends on temperature, ion mass ; If info on open vs closed not available, ; will assume all is closed ; ; keyword ANISO_OPEN -- model choice for ANISO ; not used if set in ModSolStruct (UV spectro) ; If info on open vs closed not available, ; will assume all is closed ; ; keyword CHROMORAD -- value to use for chromospheric emission in the line ; If nonzero absolute value is used for all lines as a source of resonance scattering ; if positive then it is also added as an additional emission source below the modeled corona ON DISK ; if negative -- only used as res. scat. source, and only the coronal signal shown ON DISK ; For some of the lines, the option ULIMB not eq 0 (see above) allows this CHROMORAD ; to be scaled with a Center to Limb Variation (CLV) that can be amped up by multiplying ; by the value of ULIMB ; ; keyword CHROMOHEIGHT ; height to set chromorad (source) radiation -- default r=1 Rsun ; ; NOISE TAB ; ; CURRENTLY ONLY VISIBLE FOR CORONAL POLARIMETERS ; ; ; Keywords: ; ; DONOISE: whether or not to add photon noise ; also toggles visibility of other keywords ; ; APERTURE - aperture of telescopes ; units: centimeters ; ; INTEGRATION: time observed ; units: seconds ; ; MODEFFINT, MODEFFQUANT - efficiency associated with Modulation Cycle for Stokes I, Quantity ; This will affect the noise calculation ; and the total number of photons gathered by a telescope ; See Tomczyk technical note, pages 5 and 6 ; noise is divided by this, so it represents sqrt(moddutycycle) ; where moddutycycle is the fraction of modulation cycle time applicable ; e.g. for CoMP, standard modulation cycle is ; (Io+Qo, Io-Qo, Io+Uo, Io-Uo, Io+Vo, Io-Vo) ; so moddutycycle for I is 1, moddutycycle for Q,U,V is 1/3 ; and MODEFFINT = 1, MODEFFQUANT is 1/sqrt(3) ; but even for CoMP, one might want to choose ; MODEFFQUANT=MODEFF=1 e.g. for [Io+Vo,Io-Vo]); ; or MODEFF=1, MODEFFQUANT=1/sqrt(2) for (Io+Qo, Io-Qo, Io+Uo, Io-Uo) ; ; EFFICIENCY - expected efficiency of telescopes ; units: fraction ; ; BACKGROUND - telescope location background ; units: ppm (parts per million) ; ; ERRTRUNC ; a threshold on error to plot. ; If positive, it is relative error, so points of SNR<1/ERRTRUNC ; won't be plotted as long as NULLDATCOLOR is set ; If negative, it is absolute error, so points of photon noise LosPramsStruct Tag LosUse (identical unless DoDisk changes it to XLos) ; or AZEQUI changes 'XLOS' to 'TLOS' ; unless POS is set -- in which case ; it will integrate around X=0 plane ; ; keyword NOSTRETCH -- if set and LOSUSE=TLOS, ; will not stretch TLOS step with elongtion angle ; but rather stick to same LOSMIN and LOSINT for all ; lines of sight ; default,0 ; ; Observer's position - controls line of sight ; and defines plane of sky ; ; keyword CMER - (DEGREES) -- ; Central meridian longitude (e.g. Carrington coordinates) ; of observer. ; ; If date is not set, ; for plane-of-sky GRID, cmer default -90, so that model structure at ; zero longitude is centered at west(right) limb ; for Carrington map GRID cmer default 180 centers ; Carrington map plots on 180 ; ; ; keyword BANG (double - DEGREES) -- solar B angle ; Heliolatitude of observer ; Default zero ; ; Line of sight integration ; ; keyword LOSMIN (double - GENERALLY NEGATIVE) - ; minimum line-of-sight distance or angle ; if XLOS (SOLAR RADII) ; Default x = -.5, which is r = sqrt(2.) ; for LOS intersecting photosphere ; if TAU (RADIANS) ; Default: -pi/4 (pi/2 would be for infinite LOS) ; note xlos = 0 / tau = 0 is plane of the sky ; if TLOS (SOLAR RADII) ; Defaults as XLOS, but scaled by rpos ; (intersection of line of sight with X=0 plane of sky) ; rpos=DISTOBS*tan(elong); elong = elongation angle ; DISTOBS (see below) = distance to observer (1AU default) ; keyword LOSINT (double) - resolution along the line of sight ; if XLOS (SOLAR RADII) ; Default 0.005 ; if TAU (RADIANS) ; Default aboue 0.02 ; if TLOS (SOLAR RADII) ; Default as XLOS; scaled as in LOSMIN ; ; keyword NLOS (integer)- number of points to integrate along line of sight ; Default: number needed for symmetry about POS ; (LOSMIN may need to be tweaked) ; ; ASYMMETRY ABOUT POS IS ALLOWED but requires user input ; of all three parameters (no defaults) ; otherwise the program will assume symmetry is desired ; and modify parameters accordingly ; ; ****TO FORCE SYMMETRY ABOUT PLANE OF SKY FROM WIDGET WHEN ; CHANGING NLOS AND/OR LOSMIN -- JUST SET NLOS=0*** ; ; What to do about solar disk ; ; keyword OCCULT (double) - radial height at which to draw occulting disk ; if negative value, plot dashed line and show all points ; Default 1 Rsun (photosphere) ; Units always Rsun (even when AZEQUI set and display is elongation) ; ; keyword UPOCCULT (double) - radial height above which no data plotted ; negative plot dashed line and show all points ; Default 0 Rsun- meaning no upper occulter ; Units always Rsun (even when AZEQUI set and display is elongation) ; ; keyword DODISK (0/double) - default = 0; ; if dodisk set, properties are calculated on and integrated ; above sphere of size dodisk (dodisk=1.d0 would be the photosphere) ; ***NOT AN OPTION FOR White light coronagraph and Coronal Polarimeter observations ; ***NOTE - to turn on OCCULT, DODISK must be set to zero first** ; Units Rsun ; ;; ; keyword INCRES (0/1) - what to do above disk ; INCRES=1 means double resolution ; INCRES=0 means throw away half the points (the ones that would ; have been behind the disk) ; ; Where to position model structure ; ; keyword PHIO (double - DEGREES) allows a rotation of ; model structure in phi, useful for fitting data. ; or for Carrington maps for changing numbers on X axis ; ; By FORWARD convention, model structures ; are centered on phi=0 ; ; If you are comparing model and data, or looking from ; a viewing angle for a given day, and want to (for ; example) move a structure to a limb longitude appropriate ; to the central meridian of the day, the way to do it ; is to change PHIO rather than CMER. This way also, ; if you go back and forth between STEREO and Earth's view ; point, the central meridian will change and then you ; can see how this affects the model centered at what ; used to be the limb for the other viewpoint. ; ; For model CAVMORPH, parameter PHCS is similar to ; to PHIO (unlike THCS vs THETAO, see below). ; Except that embedded cavity and nougat central longitude ; (NOUGPHCS and CAVPHCS) do not automatically change with PHCS, ; while PHIO rotates entire structure, streamer, cavity, and nougat ; ; ; keyword THETAO (double - DEGREES) similar to PHIO, allows ; a rotation of model structure from equator to ; a latitude THETAO in heliographic coordinates. ; ***NOTE IT ACTS BASICALLY LIKE POLAR ANGLE WITH A SIGN CHANGE ; ***IN THAT THETAO=90 IS AT WEST (RIGHT) LIMB ; ***AND THETATO=-90 IS AT EAST (LEFT) LIMB ; ; By FORWARD convention, model structures are centered on ; theta=90 in heliographic coordinates. ; ; So, by choosing coordinates (THETAO, PHIO) a model ; structure is placed anywhere on the sun, and then ; an integral can be performed ; depending on the viewer's position (BANG, CMER) ; ; CAVMORPH model parameter THCS is subtly different ; from THETAO, in that it simply moves the model ; streamer center to colatitude central position THCS. ; Changing THETAO rotates everyhing, so a streamer would ; lie along a great circle,not parallel to the equator as ; it would from a change in THCS. Also, note NOUGTHCS/NOUGTOP_TH and ; CAVTOP_TH (positions of embedded cavity top and nougat center and top) do not ; automatically change with a change in THCS, whereas a change ; in THETAO rotates the entire structure, streamer, cavity, and nougat. ; ; NOTE THETAO is not really meaningful for global models ; ***so turned off for PSIMAS and AWSOM and PFSSMOD and TOMO and STRIA*** ; ; (note PHIO can still be useful for global models ; for making Carrington maps not centered on 180) ; ; NOTE also- THETAO is NOT equivalent to P angle/roll ; except for the special case of BANG=0, CMER=-90, PHIO=0 ; ; FOV TAB ; ; keyword GRIDTYPE (string - PlaneOfSky or CarrMap or UserInput) ; default PlaneOfSky ; ; keyword DISTOBS (double Rsun) ; distance of observer to Sun center ; Default 215 Rsun ; ; PLANE OF SKY ; ; keywords XXMIN,XXMAX,YYMIN,YYMAX (doubles - SOLAR RADII) ; -- size for plot ; default +/-1.5 Rsun; or +/-45 degrees if AZEQUI (see below) set ; ; keywords NGRID (integer) and NGY (integer)-- ; grid spacing and size of output plot ; (if NGY set partly overrides NGRID so that ; DX does not have to equal DY) ; ngrid default 256 for POS, 128 for LOS integrated, ; nx=ny=ngrid unless limb is set - nx=ngrid/2; ny=ngrid ; ; keyword AZEQUI (0/1) ; whether to plot in Cartesian (X-Y-Z) or Azimuthal Equidistant projection ; DEFAULT 0 (Cartesian) ; ; If PLANE-OF-SKY gridtype and POS=1 (or Physical Diagnostic): ; ; keyword LOSOFFSET (double -- SOLAR RADII) -- ; Offset from center point of LOS integration (X=0 plane if LOSUSE=XLOS Thomson Sphere if LOSUSE=TAU or LOSUSE=TLOS) ; Default 0. means at plane of sky or Thomson Sphere, ; otherwise, steps towards away along observer-sun line ; ; If DoDisk is set, POS slices plot limb at position LOSOFFSET ; and also surface of radius DoDisk. If DoDisk < LOSoffset, ; essentially this plots just the portion of the surface that lies ; in front of LOSoffset. If LOSoffset < Dodisk, it plots the portion ; of the plane slice at distance DoDisk that is unobstructed by the ; spherical surface of radius DoDisk. ; ; CARRINGTON MAP ; ; [keywords XXMIN,XXMAX,YYMIN,YYMAX (doubles -- DEGREES)] ; for now -- these are not explicitly set ; so standard Carrington map is used, i.e. ; xxmin/xxmax=0/360. yymin/yymax=0/180. ; ; keywords NGRID (integer) ; ngrid default 180 (makes 2*NGrid,NGrid+fix(1./dang) ; (phi,theta) grid -- for ngrid=180 dang will be just ; under 1 so 181 degrees in latitude. Only will ; be exactly ngrid degrees in latitude for ; lower resolution. ; ; keyword RHEIGHT (double -- SOLAR RADII) - Height where data is extracted ; ; keyword LIMB ('Cmer'/'East'/'West') -- which limb or central meridian ; to extract slices from ; Note - longitude in the maps refers to the central meridian ; longitude but the data is "extracted" at the limb - ; so there is a +/- 90 degree rotation in making the maps ; if East or West ; CMER is a special case and the integration is actually done ; above central meridian. Not allowed for Coronal Polarimeter ; and White Light Coronagraphs. ; THERE WILL BE DIFFERENCES in EAST vs WEST Carrington maps ; if solar B angle interacts with angled structures; ; THERE WILL ALSO BE DIFFERENCES to vector quantities ; limb default 'West' ; ; ; PLOT TAB ; ; ; keyword PLOTLOG (0/1) - plot in log scale ; ; keyword UNITS CORONAL POLARIMETER I, Q, U, V: ; if set to 'ERG/CM2/S/SR', CoMP type data will ; be plotted as in CLE (Judge&Casini) code, ; other choices are 'ERG/CM2/S/ARCSEC2', ; if set to 'PPM' (default) will provide in units in ; parts-per-million (PPM) of Sun central brightness ; at central wavelength ; ; NOTE -- PPM is in units relative to Bsun_center ; (Sun central brightness for a given wavelength), ; and so is independent of telescope. ; For cases ERG/CM2/S/SR and ERG/CM2/S/ARCSEC2 ; NO TELESCOPE INFORMATION will be taken into consideration. ; However, PHOTONS will be calculated taking into ; consideration telescope information in ObsPramsStruct.NoisePrams ; and having it set should open the DoNoise widget ; ; NOTE -- for DATA, for now since we are not calculating equivalent ; width for CoMP data we do not allow conversion of I, Q, U, V ; from PPM for DATA ; ; WARNING: when plotting e.g. V/I or L/I units cancel out. ; ; WL Coronagraphs -- ('10^-8 Bsun_center, 1-^-8 Bsun_mean') ; ; EUV/XRAY imagers -- ('DN/S/DETPIX, DN/S/MAPPIX') ; DN/S/DETPIX is relative to detector pixel size, so, ; changing resolution (e.g., NGRID, NGY) will not change ; value of intensity of model or data plotted. ; Every instrument will have a different detector pixel ; size (DETPIX), and these are defined in ; OBSERVABLES/FOR_DETPIX_LOOKUP.PRO. ; ; DN/S/MAPPIX is relative to map pixel size, so ; this will change with NGRID/NGY. However, for ; this every similar type observations (e.g., ; 171 Angstrom intensity in any of the EUV imagers) ; will be the same scaling from instrument to instrument ; ; keyword COLORTABLE - show color bar intensity ; ; keyword SUNEDGE (double) - set to draw yellow sun outline at r=Rsun ; (A WIDGET OPTION FOR PLANEOFSKY only, and FORCED TO EQUAL ; DODISK IF DODISK SET SO DOES NOT APPEAR IN WIDGET) ; ; keywords IMAX, IMIN (doubles) - max and min for intensity ; These will default to the min and max of data in FOR_PLOT ; For now we give them 'scaled to data' input ; ; keywords NWINX/NWINY (integers) - size of window ; Default 750/750 for Plane of sky, 720/360 for Carrington map ; **NOTE since aspect ratio of 2:1 is forced for Carrington map, ; NWINY is not displayed in widget. ; ; keyword USECOLOR (integer) - color table value ; Default 0, greyscale ; Then standards like 3 (heatscale) ; - can also use red/blue (42) for ; positive/negative data; warning dont do plotlog if so! ; (can also use 41 - which is red/blue negative/positive) ; Also 7777 for AIA colortables ; (will choose based on value of keyword LINE) ; If 7777 listed for non-AIA, will do AIA 193 color ; ; keyword AXISCOLOR (integer) color of axis ; keyword BGCOLOR (integer) color of background -- 0 black, 1 white ; ; keyword CHARSIZE, CHARTHICK (double) ; ; keyword WHITEDISK (integer) - plots occulting disk in ; white/color instead of black ; (ONLY A WIDGET OPTION FOR PLANEOFSKY, and ONLY IF DODISK=0) ; Default = 'null' means does not plot a disk - so will be central color of color bar ; change to 0 for black, 1 for white... ; ; keyword NULLDATACOLOR (integer) -- nulldata color ; Default = '' will be central color of color bar ; 0 black; 1 is white, others are rainbow ; if set to negative, will not plot noisy data (see ERRTRUNC in NOISE TAB) ; ; keyword TITLE,XTITLE,YTITLE (string) ; SET TO 'ZZ' TO BE BLANK ; ; keyword NOBANGLETITLE ; don't plot B ANGLE and CMER in plot title ; ; keyword ADDTURBTITLE ; display spatial resolution of turbulence for model 'TURBHY' in title ; ; DOCONT TAB ; ; keyword DOCONT (0/1/2) - add contours ; docont = 0 no contours ; docont = 1 contours on image ; docont = 2 (or higher) contours but no image ; ; default contours for PLANEOFSKY, no contours for CARRMAP ; ; ; keyord NOCONTCOLOR (0/1) - dont use color for contours ; ; ; keyword NoCLABEL (0/1)- don't put labels on contours ; ; keyword NLEV (integer) number of contour levels ; ; keywrod C_CHARSIZE (double) size of contour label -- default is 2/3 of plot label size ; ; ; FIELDLINES TAB (only there for models with magnetic fields) ; ; keyword FIELDLINES (0/1) - overplot with small ; fieldline vectors (plane-of-sky component of magnetic field) ; Other keywords appear when FIELDLINES box selected ; (PLANEOFSKY only) ; ; keyword BSCALE (double) - Scale factor for the vector ; overplot of fieldlines ; DEFAULT is 1 -- scaled to data ; set to 0 for uniform length, negative number ; to adjust uniform length ; and positive number to adjust scaled-to-data length ; ; keyword BCOLOR (integer) - color of fieldlines ; Default red ; ; keyword BTHICK (double) - thickness of vectors ; Default 1 ; ; keyword BMINUSE (double) - minimum field strength of ; plane of sky field to plot vector for ; ; keyword NARROW (integer) ; spacing of vectors ; note number of points to skip varies with grid size, ; thus ngrid/nsarrow is number of points to skip. ; ; STKLINES TAB (only for Coronal Polarimeter observables) ; ; keyword STKLINES (0/1) - overplot with linear polarization vectors ; (subject to 180 degree ambiguity and 90 degree ambiguity ; across Van Vleck angle) ; Other keywords appear when STKLINES box selected ; ; keyword PSCALE (double) - The scale factor for plotting ; the fieldline vector onto ; the plane of sky ; if set to zero, does fixed length lines, if less than zero, ; scales to absolute value (but fixed length), ; if greater than zero then field line length reflects ; POS strength, scaled by Pscale ; ; keyword STKCOLOR (integer) - color of vectors (default green) ; ; ; keyword STKTHICK (double) - thickness of vectors (default 1.5) ; ; keyword SMINUSE (double) -- minimum magnitude of plane of sky ; to plot vector ; ; keyword NSTARROW (integer) ; spacing of vectors ; note number of points to skip varies with grid size, ; thus ngrid/nsarrow is ; number of points to skip. ; ; keyword ARROWAVE (0/1) ; arrowave will average over skipped data in ; creating arrow length and direction ; default is no averaging ; (mostly useful for data plotting)