;+ ; PROJECT ; ; Part of this program was developed within CHIANTI-VIP. ; CHIANTI-VIP (Virtual IDL and Python) is a member of the CHIANTI family ; mantained by Giulio Del Zanna, to develop additional features and ; provide them to the astrophysics community. ; ; CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of ; Astrophysical Plasmas. It is a collaborative project involving the ; University of Cambridge, Goddard Space Flight Center, and University of Michigan. ; ; NAME: ; ; CH_AIA_RESP() ; ; PURPOSE: ; ; To compute the SDO AIA temperature responses of the six coronal ; channels for a specific date. ; ; CATEGORY: ; ; CHIANTI; emissivity. ; ; EXPLANATION: ; ; This routine calculates the SDO AIA temperature responses of the six coronal ; channels. The routine first obtained the time-dependent AIA ; effective areas from the AIA SSW, then calculates CHIANTI ; isothermal spectra between 10^4 and 10^8 K and between 25 and ; 900 Angstroms, at a 0.1 resolution, either at constant denity ; or constant pressure. Note that due to the ; off-band AIA sensitivity, significant emission in some bands ; comes from wavelengths above 450 Angstroms, which were not ; originally included. Also note that the CHIANTI model for these ; longer wavelengths is not very accurate. ; The isothermal spectra are then multiplied by the effective ; areas and integrated over wavelength to produce the temperature ; responses. ; ; CALLING SEQUENCE: ; ; AIA_RESP=CH_AIA_RESP(time) ; ; EXAMPLE: ; ; To reproduce responses close to the AIA ones which were calculated ; with CHIANTI v.7.1: ; ; AIA_RESP= ch_aia_resp('20100522', pressure=1e15, $ ; abund_name=!xuvtop+'/abundance/sun_coronal_1992_feldman_ext.abund',$ ; ioneq_name=!xuvtop+'/ioneq/chianti.ioneq') ; ; INPUTS: ; ; TIME ; The time of the observations, passed to the AIA routines. ; ; PRESSURE ; The pressure, assumed to be in K * cm^-3. ; ; DENSITY ; The density, assumed to be in cm^-3. ; ; ; OPTIONAL INPUTS: ; ; ABUND_NAME The name of a CHIANTI abundance file. ; ; IONEQ_NAME: Name of the ionization equilization name to use. If not ; passed, then the user is prompted for it, unless the ; ADVANCED_MODEL is used. ; ; **** Note: if (by default) the ADVANCED_MODEL is used, ; IONEQ_NAME will be the name of the file where the new ; ion charge states are written. ; ; IONEQ_LOGT: an array of log T [K] values, defining the grid for the ; calculation, unless the isothermal option is called, or ; an ion fraction file is used. ; ; ; ATMOSPHERE: A file with the H,He abundances as a function of temperature. ; By default, the file avrett_atmos.dat is read, with data from ; Avrett E.H., Loeser R., 2008, ApJ, 175, 229 ; ; HE_ABUND: The total helium abundance relative to hydrogen. ; ; ; OUTPUT: ; An IDL structure, containing: ; ; TEMPERATURES ; the array of temperatures ; COMMENT ; a comment on what parameters were used for the calculation. ; RESP_X ; the response for the X channel ; ; KEYWORDS: ; ; ADVANCED_MODEL: include density-dependent (and CT) effects. ; ; CT: include charge transfer in advanced models ; ; NO_AUTO: If set, then the autoionization rates (contained in ; the .auto file) are not read. The autoionization states are not ; included in the calculations, i.e. a single ion rather than the ; two-ion model introduced in version 9 is calculated. This speeds ; up the calculations without affecting the lines from the bound states. ; ; DR_SUPPRESSION: Switch on DR suppression from Nikolic et al (2018) for all ions ; not included in the advanced models. The comparison with Summers (1974) suppression ; has not been checked for other elements when preparing the models. ; ; ; CALLS: ; AIA_GET_RESPONSE (AIA), ISOTHERMAL (CHIANTI), INTERPOL (IDL) ; ; HISTORY: ; Version 1, Giulio Del Zanna, 2018 Dec 5 ; ; ; v2, 1-jul-2024, Giulio Del Zanna ; ; Modified for the ionization equilibrium advanced models. ; ; ; VERSION : 2 ; ;- function ch_aia_resp, time, pressure=pressure, density=density, $ abund_name=abund_name, ioneq_name=ioneq_name, verbose=verbose,$ no_auto=no_auto,ioneq_logt=ioneq_logt, advanced_model=advanced_model,ct=ct,$ atmosphere=atmosphere,he_abund=he_abund,dr_suppression=dr_suppression if n_elements(density) gt 0 and n_elements(pressure) gt 0 then begin print,' % CH_AIA_RESP: Error, you need to define either a constant density or constant pressure' return, -1 end if n_elements(density) eq 0 and n_elements(pressure) eq 0 then begin print,' % CH_AIA_RESP: Error, you need to define either a constant density or constant pressure' return, -1 end ssw_path,/aia ; Solid angle of one AIA pixel: sterad_aia_pix=8.4d-12 ; Get the time-dependent AIA effective areas: aia_resp = aia_get_response(/dn,/area, evenorm=0, timedepend_date=time) verstr=ch_get_version() comment='AIA responses calculated in the 25-900 Angstrom range with CHIANTI version '+$ verstr+' data ' if n_elements(density) gt 0 then $ comment=[comment, ' at a fixed density= '+ trim(density)] else $ if n_elements(pressure) gt 0 then $ comment=[comment, ' at a fixed pressure= '+ trim(pressure)] ;logt=indgen(81)*0.05+4.0 logt=indgen(26)*0.1+5.0 temp = 10.^logt isothermal, 25, 900, 0.1, temp, lambda,spectrum,list_wvl,list_ident,$ pressure=pressure, edensity=density,/photons,/cont , $ abund_name=abund_name, ioneq_name=ioneq_name, verbose=verbose,$ no_auto=no_auto,ioneq_logt=ioneq_logt, advanced_model=advanced_model,ct=ct,$ atmosphere=atmosphere,he_abund=he_abund,dr_suppression=dr_suppression comment=[comment, ' with the elemental abundance file: '+abund_name] comment=[comment, ' with the ionisation equilibrium file: '+ioneq_name] eff_94=interpol(aia_resp.a94.ea, aia_resp.a94.wave, lambda) eff_131=interpol(aia_resp.a131.ea, aia_resp.a131.wave, lambda) eff_171=interpol(aia_resp.a171.ea, aia_resp.a171.wave, lambda) eff_193=interpol(aia_resp.a193.ea, aia_resp.a193.wave, lambda) eff_211=interpol(aia_resp.a211.ea, aia_resp.a211.wave, lambda) eff_335=interpol(aia_resp.a335.ea, aia_resp.a335.wave, lambda) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_94 resp_94=total(sp_conv,1) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_131 resp_131=total(sp_conv,1) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_171 resp_171=total(sp_conv,1) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_193 resp_193=total(sp_conv,1) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_211 resp_211=total(sp_conv,1) sp_conv= spectrum & sp_conv[*,*]=0. for i=0,n_elements(temp)-1 do $ sp_conv[*, i]= sterad_aia_pix*spectrum[*, i] * eff_335 resp_335=total(sp_conv,1) resp={temperatures:temp,comment: comment, $ resp_94:resp_94,resp_131:resp_131,resp_171:resp_171, $ resp_193:resp_193,resp_211:resp_211, resp_335:resp_335} return, resp end