This page was created by the IDL library routine
mk_html_help. For more information on
this routine, refer to the IDL Online Help Navigator
or type:
? mk_html_help
at the IDL command line prompt.
Last modified: Tue Jan 4 12:52:37 2011.
NAME
BRANCHING_RATIOS
PROJECT
CHIANTI
EXPLANATION
For the specified ion this routine computes branching ratios
(these are ratios between two lines that emitted from the same
upper level; such ratios are insensitive to plasma conditions).
INPUTS
ION The name of the ion in CHIANTI format. E.g., 'fe_13'.
OPTIONAL INPUTS
PATH By default the routine uses ion data from the
user's CHIANTI distribution. By setting PATH=
the user can directly specify a path to the data
files.
WRANGE Only branching ratios in the specified wavelength range are
printed.
EXTINCT Specify the interstellar extinction, E(B-V), to modify the
branching ratio value. The IDL astronomy routine FM_UNRED
is used to calculate the extinction.
LEVEL Only show branching ratios from the specified level.
MAXLEV Only show data for levels up to and including MAXLEV.
KEYWORDS
PHOTONS By default the branching ratios are given in energy units.
Setting this keyword gives them in photon units.
ALL By default the routine only shows ratios > 0.001. By
setting /ALL all branching ratios are shown.
CALLS
READ_WGFA_STR, READ_ELVLC, ION2FILENAME, FM_UNRED
EXAMPLE
IDL> branching_ratios,'fe_13',lev=20
Wavelength Ratio Lower level
Upper level 20 3s2.3p3d 3P1
202.044 1.000 1 3s2.3p2 3P0
205.915 0.006 2 3s2.3p2 3P1
209.919 0.150 3 3s2.3p2 3P2
223.777 0.015 4 3s2.3p2 1D2
HISTORY
Ver.1, 4-Nov-2003, Peter Young
Ver.2, 30-Apr-2007, Peter Young
introduced /NEG keyword, and corrected bug
Ver.3, 13-Feb-2009, Peter Young
switched to using read_wgfa_str; modified the printed output;
added LEVEL= and MAXLEV= keywords.
(See ratios/branching_ratios.pro)
Project : SOHO - CDS
Name : CHIANTI_NE
Purpose : Calculate and plot CHIANTI density sensitive line ratios.
Explanation : CHIANTI_NE (density ratios)
calculates and plots density sensitive line ratios based on
the CHIANTI atomic database of Dere et. al.
Use : IDL> chianti_ne
Inputs : None
Opt. Inputs : None
Outputs : None
Opt. Outputs: None.
Keywords : None
Calls : CALC_DMM_DR, plot_dmm_dr_fig , make_ion_list
Common : dmm_dr_com dmm_lines(with plot_dmm_dr_fig),
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : Started life as 'density_ratios' by Ken Dere
Written : C D Pike, RAL, 13-Jan-96
Modified : Added selection of els/ions from master file. CDP, 21-Jan-96
Added hardcopy of line list, refs etc. CDP, 22-Jan-96
Include multiple lines in ratio. CDP, 27-Jan-96
General upgrade and added temp/unit selections. CDP, 6-Jun-97
Added intensity ratio selection. CDP, 17-Jul-97
Added wavelength ranges. CDP, 18-Jul-97
Fixed typos introduced in version 7. CDP, 22-Jul-97
Float the user-supplied Log Temperature. CDP, 1-Aug-97
Update for IDL v5.2. CDP, 20-Apr-99
v. 11 Update list of elements. CDP, 18-Jun-99
V.12. Added ratio plots and hardcopies in linear scale, added various
checks and minor things. Added a few tags to the
ratio output structure (temperature, units, comment).
Removed optional output structure.
Updated to be CHIANTI v.3-compatible.
Giulio Del Zanna, DAMTP, 7-Oct-2000
Version 13, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
V. 14, 1-May-02, GDZ, commented out a few refs.
V. 15, 21-May-2002, GDZ, changed the way to deal with fonts.
V.16, 17-Sep-2002 (GDZ)
added !p.multi = 0 upon exit and added X-label.
Version : Version 16, 17-Sep-2002
(See ratios/chianti_ne.pro)
Project : SOHO - CDS
Name : CHIANTI_TE
Purpose : Calculate and plot CHIANTI temperature sensitive line ratios.
Explanation : CHIANTI_TE (temperature ratios)
calculates and plots temp. sensitive line ratios based on
the CHIANTI atomic database of Dere et. al.
Use : IDL> chianti_te
Inputs : None
Opt. Inputs : None
Outputs : None
Opt. Outputs: none.
Keywords : None
Calls : CALC_DMM_TR, make_ion_list
Common : dmm_tr_com
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : Started life as 'temperature_ratios' by Ken Dere
Written : H.E. Mason, 3 Oct 1996
Modified : Update for IDL v5.2. CDP, 20-Apr-99
V.3. Update list of elements. CDP, 18-Jun-99
V.4 , Giulio Del Zanna (DAMTP), 10 Oct-2000
Rewritten completely, adding possibility to select the density
at which the intensities are calculated, making this routine
compatible ith CHIANTI v.3, and with the same characteristics as
CHIANTI_TE. Added ratio plots and hardcopies in linear scale, added various
checks and minor things. Added a few tags to the
ratio output structure (density, units, comment).
Removed optional output structure.
Version 5, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
V. 6, 1-May-02, GDZ, commented out a few refs.
V.7, 21-May-2002, GDZ, fixed a bug with the fonts.
V.8, 17-Sep-2002 (GDZ)
added !p.multi = 0 upon exit and added X-label
Version : Version 8, 17-Sep-2002
(See ratios/chianti_te.pro)
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
DENSITY_RATIOS
PURPOSE:
to calculate line intensity ratios as a function of electron density
CATEGORY:
scientific analysis
CALLING SEQUENCE:
DENSITY_RATIOS,Ion,Wmin,Wmax,Dmin,Dmax,Density,Ratio,Description
INPUTS:
Ion: the CHIANTI style name of the ion, i.e., 'c_5' for C V
wmin: minimum of the wavelength range of interest in Angstroms
wmax: maximum of the wavelength range of interest in Angstroms
dmin: log10 of the minimum desired density (8. = 10^8 cm^(-3) )
dmax: log10 of the maximum desired density range
INTERACTIVE INPUTS:
Must select the line for the numerator and denominator
It is possible to select multiple lines to be summed
KEYWORD PARAMETERS:
OUTFILE: the (optional) name of the output ascii file where a
listing of the line ratio intensity as a function of
density is saved. For example, outfile='den_rat.lis'
PSFILE: the (optional) name of the output postscript file
where a plot of the choses density sensitive line
ratio is saved. For example, psfile='den_rat.ps'
TEMP: to specify the temperature, otherwise the temperature at
the peak
of the ionization equilibrium is used. For example,
temp=1.e+6
/PHOTONS: if set, the ratio will be in photon units, as opposed
to ergs
RADTEMP Specify background radiation 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.)
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
VERBOSE To print out information about the lines.
OUTPUTS:
Density: an array of the density values for which the selected
intensity ratio calculated
Ratio: an array of line intensity ratios
Description: a string describing the transitions selected
Plots the intensity ratio of the selected line as a function of density
COMMON BLOCKS:
None.
CALLS
EMISS_CALC, ION2SPECTROSCOPIC, CONVERTNAME, READ_IONEQ,
CH_XMENU_SEL
EXAMPLE:
density_ratios,'o_5',1000.,1500.,8.,13.,den,rat,desc
choose the ratio of 1371.294 to 1218.393
MODIFICATION HISTORY:
Written by: Ken Dere
March 1996: Version 2.0
May 28, 1996: Ken Dere added psfile keyword/option
Sept 1996: modified to work with VMS
and added keyword TEMP, Ken Dere
Feb. 2000: Modified for Version 3, K. Dere
14-Jul-2000 Peter Young, now calls pop_solver
26-Sep-2001 Modified for 9-point splines and proton rates;
added radtemp and rphot keywords for photoexcitation.
20-Nov-2001 Routine now calls emiss_calc to get emissivities.
V.9, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
V.10, 1-Aug-02 GDZ
Changed all the formats.
V.11, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables.
V.12, 15-Aug-02, GDZ
Major revision:
-Added the keyword VERBOSE, to avoid printing out long lists of lines.
-Removed the call to ch_xselect_s, that did not work for long lists.
-Added a '*' in the line lists, to identify 'unobserved' lines.
-Replaced the commands to create PS file, to make it
cross-platform compatible.
-Added a large number of cosmetics, mainly lables to the axes and
titles, that were missing.
-Removed plotting in windows already present.
-Added the CHIANTI version number in the outputs.
V.13, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
VERSION : 13, 3-Nov-03
(See ratios/density_ratios.pro)
PROJECT
CHIANTI http://wwwsolar.nrl.navy.mil/chianti.html
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
NAME
dens_plotter
PURPOSE:
A widget-based routine to allow the analysis of density sensitive
ratios. **** See RATIO_PLOTTER for details. *****
CALLING SEQUENCE:
IDL> dens_plotter, name,$
EM, PATH=PATH, NOPROT=NOPROT, $
IONEQ_FILE=IONEQ_FILE, ABUND_FILE=ABUND_FILE
INPUTS:
The ion name (e.g. 'si_3' for Si III)
OPTIONAL INPUTS : none
OUTPUTS:
OPTIONAL OUTPUTS:
EM: Save the displayed emissivities to structure EM.
**** See RATIO_PLOTTER for details. *****
KEYWORDS:
PATH: Data in the CHIANTI format that is not in the CHIANTI
database can be read by specifying the directory in which
it lies through PATH.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
CALLS: CONVERTNAME RATIO_PLOTTER
COMMON BLOCKS: none
RESTRICTIONS:
SIDE EFFECTS:
CATEGORY:
spectral synthesis.
EXAMPLE:
IDL> dens_plotter, 'si_9'
WRITTEN :
Ver.1, 18-Apr-2002, Giulio Del Zanna (GDZ) written as a wrapper
routine to call RATIO_PLOTTER.
MODIFIED: V.2, 2-Aug-2005, GDZ
Now the routine handles the dielectronic case
VERSION : 2, 2-Aug-2005
(See ratios/dens_plotter.pro)
Project : SOHO - CDS
Name : PLOT_CHIANTI_NE
Purpose : Plots a density sensitive ration saved from CHIANTI_NE
Explanation : The routine CHIANTI_NE allows the calculated ratio to be
saved in an IDL save file. This routine retrieves and
plots the ratio.
Use : IDL> plot_chianti_ne, file, data
Inputs : file - save file name (an extension of .CH_NE will have
been added, specifying this is optional)
Opt. Inputs : None
Outputs : None
Opt. Outputs: data - returns the retrieved ratio structure
Keywords : log. If set, a log-log plot is produced.
Calls : print2d_plot
Common : None
Restrictions: None
Side effects: None
Category : Synthetic spectra
Prev. Hist. : None
Written : C D Pike, RAL, 7-Oct-96
Modified : v.2 Added a few extra things, including possibility to create a
postscript file.
Giulio Del Zanna (DAMTP), 10-Oct-2000
Version : Version 2, GDZ 10-Oct-2000
(See ratios/plot_chianti_ne.pro)
Project : SOHO - CDS
Name : PLOT_CHIANTI_TE
Purpose : Plots a temperature sensitive ratio saved from CHIANTI_TE
Explanation : The routine CHIANTI_TE allows the calculated ratio to be
saved in an IDL save file. This routine retrieves and
plots the ratio.
Use : IDL> plot_chianti_te, file, data
Inputs : file - save file name (an extension of .CH_TE will have
been added, specifying this is optional)
Opt. Inputs : None
Outputs : None
Opt. Outputs: data - returns the retrieved ratio structure
Keywords : log. If set, a log-log plot is produced.
Calls : None
Common : None
Restrictions: None
Side effects: None
Category : Synthetic spectra
Prev. Hist. : None
Written : C D Pike, RAL, 7-Oct-96
Modified : v.2 Added a few extra things, including possibility to create a
postscript file.
Giulio Del Zanna (DAMTP), 10-Oct-2000
Version : Version 2, GDZ 10-Oct-2000
(See ratios/plot_chianti_te.pro)
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: RATIO_PLOTTER
PURPOSE:
A widget-based routine to allow the analysis of density or
temperature sensitive ratios.
EXPLANATION:
RATIO_PLOTTER is designed to study temperature and density
sensitive line ratios. For temperature ratios, just use the
keyword /temp; for density ratios just use /dens.
The routine allows line ratios relative to a
particular line (called the 'denominator line') to be viewed. One
can either choose a particular numerator, or one can simply view
all ratios within a specified wavelength range (see the button widget
just above the main plot window).
In the former case, the numerator line can be chosen either from the
strongest lines, or from all lines within a specified wavelength
range.
A wavelength range is selected via the sliders at the lower left of
the main widget.
A default set of emissivity parameters is used initially to create
the first plot that you see. To change the parameters, click on the
'CHANGE PARAMETERS' button near the top of the GUI. This activates
a new set of widgets allowing the user to change whether energy or
photon units are needed, whether proton rates are included, the
temperature/density range, etc. Note that while the parameters are
being changed, the user can not modify the line selection or plot
parameters.
When a particular numerator line has been selected, observed
intensities (and error bars) for both the denominator and numerator
can be input, and the derived density (plus error bars) can be seen
on the plot (click on 'PLOT ERROR BARS'), or in a text widget (see
the 'SHOW DERIVED DENSITIES' button).
The accuracy of the derived density or temperature is limited by the
intervals in the emissivity calculation. The intervals can be
changed on the widget (there are 4 choices given) and if a new
interval is selected, new emissivities should be calculated.
Using the smallest intervals will give the highest accuracy for
the computed density or temperature.
CALLING SEQUENCE:
RATIO_PLOTTER, IZ, ION [, /TEMP, /DENS, EM, PATH=, /NOPROT, $
IONEQ_FILE=, ABUND_FILE= ]
EXAMPLES:
RATIO_PLOTTER, 26, 13, /TEMP ; Fe XIII
RATIO_PLOTTER, 10, 6, /DENS ; Ne VI
RATIO_PLOTTER, 26, 13, /DENS, PATH='/home/new_chianti_data'
INPUTS:
IZ: The atomic number of the ion
ION: The spectroscopic number of the ion (e.g., 12 = XII)
OPT. INPUTS:
EM: Save the displayed emissivities to structure EM. This
structure is simply the structure EMISS_SELECT used in
the routine, with some extra tags. This structure has the
tags:
.lines.emiss Emissivities of line at requested densities
.lines.wavel Wavelength(s) of line (blend)
.dens Log10 electron density/densities
.temp Log10 electron temperature(s)
.rphot Photoexcitation radius
.radt Radiation temperature
.proton String indicating whether proton rates are
included.
.date The date and time at which structure was
created.
.version The version of CHIANTI that created the
structure.
PATH: Data in the CHIANTI format that is not in the CHIANTI
database can be read by specifying the directory in which
it lies through PATH.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
KEYWORDS:
DENSITY If set then ratios are plotted as a function of
density rather than temperature.
TEMPERATURE If set then the ratios are plotted as a function of
temperature rather than density.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
PROGRAMMING NOTES:
RATIO_PLOTTER is actually a collection of several routines....
DENS_FINDER - converts observed ratios into densities
INDEX_EXTRACTOR - a device for extracting indices out of arrays
WAVEL_PLOT - plots the little window in bottom left of GUI
DENS_PLOT - updates the plot window
DENS_MAIN_EVENT - responds to widget actions
SAMPLE_WID - sets up the widgets
RATIO_PLOTTER - loads up various initial parameters
The emissivities of all the ion's lines are stored in the
structure "emiss", while those of the selected lines are stored
in "emiss_sel". This latter can be output into IDL by giving the
"EM" optional input on the command line.
The routine is set up to allow more than one numerator to be
displayed at once, but I've never actually found a need to
implement this yet. (Note that you'll see "Numerator 1" on
the widget.)
CALLS:
EMISS_CALC, READ_IONEQ, EMISS_SELECT, ZION2NAME,
ZION2FILENAME, ZION2SPECTROSCOPIC, PS, PSCLOSE, IS_NUMBER,
CHIANTI_FONT, TRIM
INTERNAL PROCEDURES AND FUNCTIONS
DENS_FINDER, INDEX_EXTRACTOR, DENS_PLOT, DENS_MAIN_EVENT,
SAMPLE_WID, WAVEL_PLOT
COMMON BLOCKS
EMISS_DATA, SELECT, SLIDERS, PLOTTING, RAD_DATA, PROTON_RATES,
EXTRA, ELVLC, FILES, TEMP
HISTORY:
Ver.1: PRY, 15-SEP-97.
Ver.2: PRY, 6-JUL-98, added EM and PATH
Ver.3: PRY, 5-SEP-98, added call to choose_ioneq
Ver.4: PRY, 11-JAN-99, added PROTON keyword and widget to allow
the addition of proton rates
Ver.5: PRY, 3-FEB-99, added a title to the widget, and the name
of the ion to the ratio plot title
Ver.6: PRY, 25-MAR-99, corrected bug for wavelengths > 1000
angstroms
Ver.7: PRY, 1-JUN-99, routine now works in CDS environment
without use_dere_chianti
Ver.8: PRY, 22-FEB-00, corrected colour problem
Ver.9: PRY, 17-AUG-00, added windows identifying the numerator
and denominator transitions. This required an
extra routine (MAKE_STRINGS) and a common block
(ELVLC).
Ver.10: PRY, 25-AUG-00, added buttons to allow a choice between
ratios in energy or photon units.
Ver.11: PRY, 25-AUG-00, can now specify a wavelength range by
directly typing in the numbers
Ver.12: PRY, 30-Nov-00, changed call to emiss_select
Ver.13: PRY, 21-Dec-00, removed set_plot,'x' following help from
Bill Thompson
Ver.14, PRY, 27-Dec-00, changed switch to tst1 for IDL v5.4
Ver.15, PRY, 7-Dec-01, changed /prot keyword to /noprot to be
compatible with other CHIANTI routines.
Added /temperature keyword.
Ver.16, PRY, 28-May-02, removed SPLINE calls, changing them to
SPL_INIT and SPL_INTERP; changed density labels to
temperature labels where appropriate.
Ver.17, PRY, 29-May-02, made treatment of photoexcitation consistent
with other CHIANTI routines.
V. 18, 29-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for Unix,
Windows and VMS.
Now we only call zion2filename.
When creating the ps file, ps and psclose are used.
v.19, 12-Jun-02 GDZ
fixed a small bug when finding the names of the files when the
keyword PATH is given.
v.20, 2-Aug-02, Peter Young
made some cosmetic changes following Giulio's suggestions.
v.21, 5-Aug-02, Peter Young
made various changes:
- the emissivity parameters (at top of widget) can only be
changed independently of line selection now
- the text widgets now check to make sure the user inputs
are numbers.
- extended the number of tags on the output EM structure
v.22, 6-Aug-02, Peter Young
corrected plot problem when viewing all temperature ratios
in a fixed wavelength range.
v.23, 8-Aug-02, Peter Young
a number of cosmetic changes to make the GUI more
user-friendly
v.24, 13-Aug-02, Peter Young
changed the temperature/density text widget so that numbers
are registered even if the return key has not been hit.
v.25, 14-Aug-02, Peter Young
photoexcitation button now works again; also some cosmetic
changes
V.26, 17-Sept-02, GDZ
added scrolling in main frame
V.27, 10-Feb-03, Peter Young
corrected bug related to fonts on Windows PCs
V.28, 13-Feb-03, Peter Young
corrected problem when ion balance data dosen't exist for
an ion
V.29, 18-Feb-03, Peter Young
added call to routine chianti_font to deal with fonts.
V.30, 28-Aug-03, Peter Young
corrected bug when two lines have the same wavelength by
introducing .ind tag to emiss_sel
V.31, 3-Nov-03, Giulio Del Zanna
Added printout of Ne(Te) vs. ratio values
Modified format e8.2 to e9.2 for Windows compatibility.
V.32, 6-Nov-03, Peter Young
Corrected bug when new emissivities are calculated that
prevented the emissivites in emiss_sel from being updated.
Also, the Ne(Te), ratio values are now printed to a pop-up
window through the new 'SHOW RATIO VALUES' button rather
than printed to the text window (see V.31).
V.33, 7-Nov-03, Giulio Del Zanna (GDZ)
Modified the popup widget by calling xpopup and adding
labels. Now it is possible to paste and copy the RATIO
values into a file.
V.34, 12-Dec-03, Peter Young
Lowered the position of the postscript plot on the paper so
that the title isn't chopped off on US letter-size paper.
V.35, 2-Aug-2005, GDZ
Various modifications. Now the routine handles the
dielectronic case. Added printing of line lists in the
line ratio plots. Added the option to print directly to
the PRINTER. Added the option to SAVE a structure
containing the emissivities into an IDL save file (using
SAVEGEN). Added retain=2 to the window. Added
logarithmic or linear plot switch. Added cleaning of the
variables at the start of the routine. Various minor
cosmetic changes.
V.36, 12-Aug-2005, GDZ
Reinstated some previous cosmetic features. Also adjusted
some sizes, added some checks (e.g. minimum is set to 1e-10 if
plot is in log scale -to avoid log(0)-; automatic scaling cannot
be set if log scale is on).
V.37, 15-Aug-2005, Peter Young
Corrected bug with derived densities when the theoretical ratio
is double-valued.
V.38, 15-Aug-2005, Peter Young
Corrected bug introduced by modification above.
V.39, 17-Aug-2005, Peter Young
Adjusted layout of widget, modified printing of wavelengths
in the plot window, and adjusted plot limits for log scale.
V.40, 18-Aug-2005, Peter Young
Corrected bug for temperature version of routine that led to
mismatch between stated parameters and plotted parameters
v.41, 7-dec-07, GDZ fixed two minor bugs.Allow long lists.
VERSION : 41, 7-dec-07
(See ratios/ratio_plotter.pro)
This procedure has a dual purpose: (i) to extract `emiss' indices from
`emiss_sel' and, (ii) create labels that will be displayed on the plot
window.
The lines that comprise the blend are contained in emiss_sel.label
as, e.g., '203.79+203.80'. This routine separates this string into
the separate wavelengths and looks in emiss.lambda to see which
indices they correspond to. The set of indices are output through INDEX.
INPUT
I Index of component in emiss_sel. E.g., for the denominator I=0,
for the numerator I=1.
OPTIONAL OUTPUT
INDEX Integer array of same length as the number of lines in the
numerator or denominator (based on value of I). The elements
give the indices of the lines as they appear in the EMISS
structure.
PLOT_LABEL A string containing the index to be used when labelling
the line ratio plots.
KEYWORD
PS Setting this adds an angstrom to the wavelength labels. (Only
works for the postscript device.)
(See ratios/ratio_plotter.pro)
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
TEMPERATURE_RATIOS
PURPOSE:
calculate and display temperature sensitivity of line intensity ratios
CATEGORY:
spectral diagnostics
PROCEDURE :
The intensities (Population of the upper level * A) of the lines within
the selected ion are first calculated, either at constant pressure or
at constant density (however specified in the input). They are plotted
in window 0. The intensities relative to the brightest reference line
are then plotted in window 1. A widget allows the user to select a
number of lines (at least one!) for the numerator of the ratio, and a
number of lines for the denominator. In case of multiple selections, the
line intensities are summed. The ratio values are plotted in window 2, and
optionally also saved in a text file. A postscript file can also be
created. The ratio values, calculated at twice and half the prescribed
density are also calculated and overplotted, to show how the
temperature ratio also depends on the density.
CALLING SEQUENCE:
> temperature_ratios,ion,wmin,wmax,Log10(tempmin),Log10(tempmax),temperature,ratio,description,$
[pressure= ,density= , psfile= , outfile= ]
EXAMPLE:
> temperature_ratios,'c_4',100.,1600.,4.,6.,temp,ratio,desc,density=1.e+10,$
psfile='test.ps', outfile='test.txt'
then select the ratio of (384.17 + 384.19) to 1550.772
INPUTS:
Ion: the CHIANTI style name of the ion, i.e., 'c_5' for C V
Wmin: minimum wavelength limit in Angstroms
Wmax: maximum wavelength limit in Angstroms
Tempmin: log10 of lowest temperature of interest, i.e. 4 for 10.^4 K
Tempmax: log10 of highest temperature of interest
OPTIONAL INPUTS:
Must specify indices of lines which are to form the ratio
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.)
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
OUTPUTS:
Temperature: an array of temperatures spanning Tempmin to Tempmax
Ratio: an array of the intensity ratio of the selected lines
Desc: a short string description of the selected line ratio
OPTIONAL OUTPUTS:
Ps and/or text file with the intensity ratio.
KEYWORD PARAMETERS:
DENSITY: calculates the intensity ratios for constant density.
If neither density or pressure are specified, a constant
density of 1.e+10 cm^-3 is assumed as default.
OUTFILE: the (optional) name of the output ascii file where a
listing of the line ratio intensities as a function of
temperature is saved.
PSFILE: the (optional) name of the output postscript file
where a plot of the chosen temperature sensitive line
ratio is saved.
NOPROT Switches off inclusion of proton rates.
VERBOSE prints out information
CALLS:
read_ioneq, convertname, ion2spectroscopic,ion2filename,
ch_xmenu_sel, emiss_calc
COMMON:
elvlc,l1a,term,conf,ss,ll,jj,ecm,eryd,ecmth,erydth,eref
wgfa, wvl,gf,a_value
upsilon,t_type,deu,c_ups,splups
proton, pstr, pe_ratio
radiative, radt, dilute
RESTRICTIONS:
SIDE EFFECTS: None known yet.
MODIFICATION HISTORY:
Written by: Ken Dere
May 1996: Version 2.0, Ken Dere
April 2000: V. 3 Ken Dere modified for V3
14-Jul-2000 V. 4 Peter Young, now calls pop_solver
2-Oct-2000 V. 5 Giulio Del Zanna, corrected an error in the
creation of the string list of the lines in the ratio.
Also corrected a few minor errors.
Removed the device,window_state call, and added a few
other 'cosmetic' adjustments.
Version 6, 21-Dec-2000, William Thompson
Modified for better cross-platform capability.
Ver.7, 6-Dec-2001, Peter Young
Revised to call emiss_calc for the emissivities.
V.8, 21-May-2002, GDZ
generalized directory concatenation to work for
Unix, Windows and VMS.
V.9, 1-Aug-02 GDZ
Fixed label mistake, and changed all the formats.
V.10, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables.
V.11, 15-Aug-02, GDZ
Major revision:
-Added the keyword VERBOSE, to avoid printing out long lists of lines.
-Removed the call to ch_xselect_s, that did not work for long lists.
-Added a '*' in the line lists, to identify 'unobserved' lines.
-Replaced the commands to create PS file, to make it
cross-platform compatible.
-Added a large number of cosmetics, mainly lables to the axes and
titles, that were missing.
-Removed plotting in windows already present.
-Removed the pressure keyword.
-Added the CHIANTI version number in the outputs.
V.12, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
VERSION : 12, 3-Nov-03
(See ratios/temperature_ratios.pro)
PROJECT
CHIANTI http://wwwsolar.nrl.navy.mil/chianti.html
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
NAME
temp_plotter
PURPOSE:
A widget-based routine to allow the analysis of temperature sensitive
ratios. **** See RATIO_PLOTTER for details. *****
CALLING SEQUENCE:
IDL> temp_plotter, name,$
EM, PATH=PATH, NOPROT=NOPROT, $
IONEQ_FILE=IONEQ_FILE, ABUND_FILE=ABUND_FILE
INPUTS:
The ion name (e.g. 'si_3' for Si III)
OPTIONAL INPUTS : none
OUTPUTS:
OPTIONAL OUTPUTS:
EM: Save the displayed emissivities to structure EM.
**** See RATIO_PLOTTER for details. *****
KEYWORDS:
PATH: Data in the CHIANTI format that is not in the CHIANTI
database can be read by specifying the directory in which
it lies through PATH.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
CALLS: CONVERTNAME RATIO_PLOTTER
COMMON BLOCKS: none
RESTRICTIONS:
SIDE EFFECTS:
CATEGORY:
spectral synthesis.
EXAMPLE:
IDL> temp_plotter, 'fe_13'
WRITTEN :
Ver.1, 18-Apr-2002, Giulio Del Zanna (GDZ) written as a wrapper
routine to call RATIO_PLOTTER (written by P. Young).
MODIFIED: V.2, 2-Aug-2005, GDZ
Now the routine handles the dielectronic case
VERSION : 2, 2-Aug-2005
(See ratios/temp_plotter.pro)