;+ ; PROJECT ; ; 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. ; ; 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. ; ; ; NAME: ; ISOTHERMAL ; ; PURPOSE: ; Computes spectra from isothermal plasmas. A number of isothermal ; plasmas can be included. ; Note that this routine has a number of unique features that ; distinguish it from the other CHIANTI synthetic spectra routines. ; See the Programming Notes section. ; ; INPUTS: ; WMIN Minimum of desired wavelength range in Angstroms. ; ; WMAX Maximum of desired wavelength range in Angstroms. ; ; WAVESTEP Bin size of spectrum (in Angstroms) ; ; TEMP Electron temperature (or array). ; ; OPTIONAL INPUTS: ; ; PRESSURE Electron pressure in units of cm^-3 K. ; ; EDENSITY Electron density in units of cm^-3. ; ; EM Emission measure. The units of EM govern the intensity ; units of the emission lines (i.e., column or volume ; emission measure units). If EM is not specified, then the ; emission measure is set to (N_e * N_H) where N_e is ; derived from the user-specified PRESSURE or EDENSITY, ; and N_H is derived from the routine PROTON_DENS.PRO. ; ; SNGL_ION Rather than include the entire list of CHIANTI ions in ; the calculation, this input can be used to select a ; single ion, or a number of different ions. E.g., ; SNGL_ION='s_2' or SNGL_ION=['s_2','s_3','s_4']. ; ; RADTEMP The blackbody radiation field temperature (default 6000 K). ; ; RPHOT Distance from the centre of the star in stellar radius units. ; I.e., RPHOT=1 corresponds to the star's surface. (Default is ; infinity, i.e., no photoexcitation.) ; ; MASTERLIST The list of ions that will be considered for the ; spectrum is contained in the masterlist file in the ; CHIANTI directories. The user can specify his own file ; through this keyword. E.g., ; masterlist='/user/home/masterlist.ions' ; ; ; ABUND_NAME: Name of the abundance file to use. If not passed, then ; the user is prompted for it. ; ; 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. ; ; ; ; KEYWORD PARAMETERS: ; ; NOPROT Switch off the inclusion of proton rates in the level ; balance. ; ; ERGS The units of the output spectrum are by default in photons. ; Setting /ERGS switches to erg units. ; ; CONT Adds continuum (free-free, free-bound, two-photon) to ; spectrum. ; ; ALL Include all lines, i.e. also those for which wavelengths ; are only theoretical and not observed. ; 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. ; ; ; ; OUTPUTS: ; ; LAMBDA Wavelength array of calculated synthetic spectrum. ; ; SPECTRUM Intensity array. The units depend on the user inputs to ; ISOTHERMAL -- see note below. ; ; LIST_WVL A list of wavelengths for use with synthetic_plot.pro ; ; LIST_IDENT A list of line identifications for use with ; synthetic_plot.pro ; ; PROGRAMMING NOTES: ; ; Intensity Units ; --------------- ; The units are of the form photons cm^3 s^-1 sr^-1 * (units of EM), ; changing to ergs if the /ergs keyword is set. ; ; The volume emission measure (N_e*N_H*V) has units cm^-3. ; ; The column emission measure (N_e*N_H*h) has units cm^-5. ; ; ; Unique features ; --------------- ; The emission lines in the final spectrum have no width and thus ; each occupies a single pixel of the spectrum. The size of the ; pixels are set by WAVESTEP. ; ; As stated above, the units of the output spectrum are ; photons cm^3 s^-1 sr^-1, i.e., there is no "per angstrom" term. ; This means that (i) the height of the emission lines in the ; spectrum does not change with varying WAVESTEP, and (ii) the height ; of continuum does change with WAVESTEP. ; ; CALLS: ; CH_SYNTHETIC, READ_ABUND, CH_GET_FILE, CONCAT_DIR, FREEFREE, ; FREEBOUND, TWO_PHOTON ; ; HISTORY: ; Ver.1, 8-Apr-02, Peter Young Rutherford Appleton Laboratory, ; p.r.young@rl.ac.uk ; Tries to replicate the behaviour of the original ISOTHERMAL which ; was found in earlier versions of CHIANTI (v.3 and earlier). ; ; MODIFICATION HISTORY: ; Ver. 2, Giulio Del Zanna (GDZ), 28-Apr-02 ; Added abund_name,ioneq_name keywords. ; Also, added photons keyword in call to MAKE_CHIANTI_SPEC. ; ; Ver. 3, Peter Young, 24-May-02 ; Modified to produce arrays of spectra when an array of ; temperatures is given ; ; V.4, GDZ, 28-May-02 ; Added a couple of checks on file existence and modified the call ; to ch_synthetic and make_chianti_spec due to change of keyword ; names. ; ; V.5, Peter Young, 16-Jul-02 ; Restructured routine to avoid crashes when a large number of ; temperatures is input. ; ; V.6, 8-Aug-02 GDZ ; Added one error checking ; ; V.7, 18-Aug-03, Peter Young ; Added EM= keyword. ; ; V.8, 14-Sept-2005 GDZ ; Added ALL keyword and modified header, error message. ; ; V.9, 3-Oct-2005, GDZ ; Now the FOR loop accepts more than 32000 lines. ; ; V.10, 7-Oct-2009, Peter Young ; The keyword EM_INT is now used in the call to the ; continuum routines. ; ; V.11, 17-Aug-2015, Peter Young ; Changed 'lambda' to 'lmbda' as IDL have introduced a ; function called lambda. ; ; V.12, 5-Dec-2018, GDZ ; replaced noverbose with verbose. ; ; V.13, 20-Feb-2019, Peter Young ; Added check on TEMP to make sure it's in ; ascending temperature order; now uses !ioneq_file for ; the ion balance file if ioneq_name is not set. ; ; V.14, 26-Apr-2019, Peter Young ; Modified call to freefree - no longer uses common ; block. ; ; V.15, 01-Apr-2020, Peter Young ; Now uses abund_file and ioneq_file inputs for ; two_photon and freebound; removed the elements common ; block; updated header. ; ; v16, 1-Feb-2024, Giulio Del Zanna ; Modified for the ionization equilibrium advanced models. ; ; v.17, 06-Feb-2026, Peter Young ; For call to "fix", have added type=3 to return a long integer. ;- PRO isothermal, wmin,wmax,wavestep,temp,lmbda,spectrum,list_wvl,list_ident,$ pressure=pressure,edensity=edensity,photons=photons, ergs=ergs, $ sngl_ion=sngl_ion, abund_name= abund_name , ioneq_name=ioneq_name, $ verbose=verbose, min_abund=min_abund, cont=cont, $ masterlist=masterlist, noprot=noprot, radtemp=radtemp, $ rphot=rphot, em=em,all=all,$ 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_params() LT 6 THEN BEGIN print,'Use: IDL> isothermal,wmin,wmax,wavestep,temp,lambda,spectrum,list_wvl,' print,' list_ident, pressure= , edensity= , /photons,' print,' /verbose, sngl_ion= , min_abund= , /cont,' print,' masterlist= ,abund_name= , ioneq_name= ,/noprot]' print,' radtemp= ,rphot= ,em= , /all ' print,'' print,'E.g., IDL> isothermal,170,180,0.1,1e6,lambda,spectrum,list_wvl,'+$ 'list_ident,' print,' edensity=1e10' return ENDIF ; ; PRY, 24-Jul-2018 ; Check to make sure temp is in ascending order (if it's an array) ; chck_temp=temp[sort(temp)] k=where(chck_temp NE temp,nk) IF nk GT 0 THEN BEGIN print,'% ISOTHERMAL: the TEMP array must be in ascending temperature order. Returning...' return ENDIF IF keyword_set(ergs) THEN photons=0 ELSE photons=1 IF n_elements(spectrum) NE 0 THEN junk=temporary(spectrum) IF n_elements(min_abund) EQ 0 THEN min_abund=0. IF (n_elements(pressure) NE 0 AND n_elements(edensity) NE 0) OR $ (n_elements(pressure) EQ 0 AND n_elements(edensity) EQ 0) THEN BEGIN print,'%ISOTHERMAL: Please specify either EDENSITY or PRESSURE' return ENDIF n=n_elements(edensity) nt=n_elements(temp) IF n_elements(em) NE 0 THEN BEGIN IF n_elements(em) EQ nt THEN BEGIN logem_isothermal=alog10(em) ENDIF ELSE BEGIN logem_isothermal=alog10(em[0]) ENDELSE ENDIF ELSE BEGIN logem_isothermal=dblarr(nt) ENDELSE ; ; PRY, 24-Jul-2018 ; Get rid of widget selection for ioneq file ; ; GDZ - revert to original way, ask to choose ionization equilibrium file for transparency. ;IF n_elements(ioneq_name) EQ 0 THEN ioneq_name=!ioneq_file IF n_elements(abund_name) EQ 0 THEN BEGIN dir=concat_dir(!xuvtop,'abundance') abund_name=ch_get_file(path=dir,filter='*.abund', $ title='Select Abundance File') IF NOT file_exist(abund_name) THEN message, 'Error, no file selected -- EXIT' END IF nt NE 1 THEN no_sum_int=1 spectrum=-1 ch_synthetic,wmin,wmax,out=out, press=pressure, err_msg=err_msg, $ sngl_ion=sngl_ion,ioneq_name=ioneq_name,dem_name=dem_name, $ photons=photons, masterlist=masterlist, noprot=noprot, $ radtemp=radtemp, rphot=rphot, verbose=verbose, progress=progress, $ density=edensity, no_sum_int=no_sum_int, logt_isothermal=alog10(temp), $ logem_isothermal=logem_isothermal,all=all,$ 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 err_msg [0] NE '' THEN BEGIN print, '% ISOTHERMAL: Error - EXIT' return END nl=n_elements(out.lines) format='('+strtrim(string(nt),2)+'e10.2)' read_abund,abund_name,abund,ref nw=fix((wmax-wmin)/wavestep,type=3)+1 lmbda=findgen(nw)*wavestep+wmin spectrum=dblarr(nw,nt) str1=out.lines.snote+' '+out.lines.ident FOR i=0L, long(nl-1) DO BEGIN int=out.lines[i].int*abund[out.lines[i].iz-1] str1[i]=strpad(str1[i],50,/after)+' Int='+string(format=format,int) getmin=min(abs(lmbda-out.lines[i].wvl),ind) spectrum[ind,*]=spectrum[ind,*]+int ENDFOR list_ident=str1 list_wvl=out.lines.wvl i=sort(list_wvl) list_wvl=list_wvl[i] list_ident=list_ident[i] IF keyword_set(cont) THEN BEGIN ; em_int=double(10.)^logem_isothermal ; IF n_elements(edensity) EQ 0 THEN edensity=pressure/temp freebound, temp,lmbda,fb,min_abund=min_abund, $ photons=photons, em_int=em_int, abund_file=abund_name, $ ioneq_file=ioneq_name freefree,temp,lmbda,ff,min_abund=min_abund, $ photons=photons, em_int=em_int, abund_file=abund_name, $ ioneq_file=ioneq_name two_photon, temp, lmbda, two_phot,min_abund=min_abund, $ edensity=edensity, photons=photons, em_int=em_int, abund_file=abund_name, $ ioneq_file=ioneq_name totcont=(fb+ff+two_phot)/1d40*wavestep spectrum=spectrum+totcont ENDIF print, '% ISOTHERMAL: calculation finished' END