CHIANTI
An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.
George Mason University (USA) -
University of Michigan (USA) -
University of Cambridge (UK)
- NASA Goddard Space Flight Center (USA)
Database History
CHIANTI Database Version 10.1 and IDL
version 10.2 released,
June 2023
CHIANTI 10.1 contains updated ionization rates for 13 ions, and
updated recombination rates for the phosphorus isoelectronic
sequence. New electron collision and radiative datasets for eight
ions in the nitrogen and oxygen isoelectronic sequences have been
added, and energy level and wavelength data have been updated for
seven other ions. Full details are given
in Dere
et al. (2023, ApJS).
The IDL software features a number of bug-fixes and
improvements. The most significant is a change to how level
populations are computed, which should lead to a speed increase in
calculating synthetic spectra of around a factor five.
June 2022 - CHIANTI database version 10.0.2
released
This is a minor release, with a new directory 'em' added containing
some emission measure distributions. There were no changes to the
atomic data.
November 2020 - CHIANTI v. 10.0 released
CHIANTI 10 includes updated atomic data for most of the ions along the beryllium, carbon
and magnesium isoelectronic sequences. The helium-like ion models
have been upgraded to two-ion models to enable modeling of
recombination and autoionization processes. A new model of Fe VII
has been added that produces many lines in the extreme ultraviolet
part of the spectrum, and a number of energy levels of the coronal
iron ions Fe X-XII have been updated.
IDL software has been added to
allow the suppression of dielectronic recombination rates to be
modeled, leading to ionization fraction tables that are density
sensitive. Updated rates for Si-like ions recombining to P-like ions
have been added, along with improved recombination rates into
neutral helium.
The paper describing CHIANTI 10 was published in The Astrophysical Journal.
September 2015 - CHIANTI v. 8.0 released
CHIANTI v. 8.0 includes several new entries and revises the atomic data for
many ions. In particular, for ions of the He-like, Li-like, B-like, Ne-like and
Na-like isoelectronic sequences,
plus several important coronal iron and nickel ions.
In addition, the method for computing the
differential emission measure has been changed.
Important note:
for various reasons, it has been necessary to modify the format
of the elvlc and splups files.
The elvlc files have been restructured but retain the same name,
while the splups files have been significantly revised and are now renamed
as "scups" files. For both the updated elvlc and new scups files, an
ascii fixed text width format has been retained.
We have modified the CHIANTI software to read these new files, but all
the main software is left unchanged.
The new database and IDL programs are incompatible with the
previous CHIANTI versions and vice-versa.
August 2013 - CHIANTI v. 7.1.3 released
An error in the routine that calculates radiative recombination rates was discovered. This error mainly affected the ionization equilibrium of the neutral and first ionization stage. The new database file contains a corrected file of ionization equilibria chianti.ioneq as well as the previous version that has been renamed to chianti_v7.ioneq for those who are interested in the checking the differences.
May 2013 - CHIANTI v. 7.1.2 released
Version 7.1.1 is a bug-fix release. It corrects problems with the o_2.wgfa file that contains wavelengths, weighted-oscillator strengths and A-values.
April 2013 - CHIANTI v. 7.1.1 released
Version 7.1.1 is a bug-fix release. It corrects problems with the c_2.wgfa file that contains wavelengths, weighted-oscillator strengths and A-values.
October 2012 - CHIANTI v. 7.1 released!
The main feature of CHIANTI Version 7.1 is the inclusion of a large
number of configurations to the atomic models of Fe VIII to XIV. These
configurations give rise to a forest of spectral lines in the 50-170 A
wavelength range that contribute significantly to the total radiative
output of the Sun at those wavelengths. Also, they give rise to several
strong lines that are currently neglected by spectral codes, and provide
significant contributions to the SDO/AIA bandpasses centered at 94A
and 131A. These data are calculated using the Flexible Atomic Code
(FAC) under the distorted wave approximation.
Additional data for a few more ions are included, that improve
the available datasets for a few ions, and correct a few glitches for
other ions at all wavelength ranges. New element abundance data
sets are provided, and improved recombination rates are included
and used to provide a new set of CHIANTI ionization equilibria
(chianti.ioneq file).
October 2011 - CHIANTI v. 7 released!
We would like to announce the release of version 7.0 of the CHIANTI
database for astrophysical spectroscopy. With Version 7.0, CHIANTI
now includes data for several new ions as well as significant updates to
many ions, including several key Fe species routinely observed by
Hinode/EIS and SDO. Also, a completely new implementation of the
CHIANTI software in the Python programming language has been
developed and is freely available on the web -- ChiantiPy.
January 2010 - CHIANTI team receives award from the Royal Astronomical Society!
On January 8 2010 the CHIANTI team were awarded the Group Achievement Award
for Geophysics by the Royal Astronomical Society (UK). The citation was:
"The Group Achievement Award for Geophysics is given to the CHIANTI consortium, the team of
scientists who have developed the 'Atomic Database for Spectroscopic Diagnostics of Astrophysical
Plasmas.' This is a powerful tool for scientists who use the dispersion of light by wavelength
(spectroscopy) to measure the properties of astronomical objects, including their composition,
temperature, density and magnetic field strength. The analysis requires detailed knowledge of
a large range of atomic elements. The CHIANTI consortium's achievement is the establishment
of a systematic, easy-to-use and publically available database to assist this process, with
a huge impact on solar and stellar physics."
A full press release is available from the RAS website.
October 2009 - CHIANTI v. 6.0.1 released!
We found an error in the continuum routines: the routines assumed that in the DEM input
the temperatures were specified at intervals of logT=0.1. An arbitrary interval is now
allowed. With the previous versions of the continuum routines, if the user specified the
CHIANTI.IONEQ ion balance the result would be a continuum that is a factor two too high
since the DEM would be tabulated at 0.05 dex intervals whereas the continuum routines
would be expecting 0.10 intervals.
Version 6.0.1 corrects this error. The error only affected calculations done using the
CHIANTI.IONEQ ion balance, and it did not affect calculations done with earlier versions
of the database.
The routines should now yield the same continuum as calculated in version 5.2
and earlier. CHIANTI 6 saw the first release of an ion balance file
(chianti.ioneq) for which the temperature spacing was 0.05 dex (in log T)
rather than the usual 0.10. A temperature spacing of 0.10 had been hardcoded
in the continuum routines, and so the derived continuum when using the
chianti.ioneq file became a factor 2 larger than it should have been. (Note
that the 0.10 spacing was not hardcoded for emission line calculations and
so these are unaffected.) This bug has been fixed, and the changes will be
transparent if you use ch_ss, ch_synthetic and make_chianti_spec for
generating synthetic spectra.
If you directly call the CHIANTI continuum routines (freefree, freebound,
two_photon) please note that a new keyword has been introduced called
EM_INT. If you are modelling an isothermal plasma, you should use EM_INT to
specify the emission measure value. If you are modelling a plasma with a
differential emission measure curve you should specify the DEM values
through the keyword DEM_INT. Previously the user would have to specify
emission measures by manually converting them to DEM values and then
inputting them via DEM_INT.
An error was also corrected in the calculation of the correction factor
to include ionization and recombination effects into level populations.
Such error only affected results at very low densities, when collisional
excitation becomes very small.
A few minor typos were also corrected in cr_7.wgfa, mn_8.wgfa, fe_18.cilvl
and fe_18.reclvl files.
July 2009 - CHIANTI v. 6 released!
We would like to announce the release of the version 6.0 of the CHIANTI database for astrophysical
spectroscopy. With Version 6, CHIANTI includes ionization and recombination coefficients for the
calculation of ion fractions, as well as software to read and handle them. CHIANTI 6.0 also
improves the calculation of He-like line intensities, and renews the data for the Be-like and F-like
sequences and for the key ions Fe XVIII and Fe XX. Data for many other ions have been updated and
new ions have been added to the database. Ion fraction datasets from recent calculations are also
included.
The main changes in the data consist of the renewal of the data of Fe XVIII and XX to improve the
calculation of a large number of lines in the X-rays, n=3,4 configurations in the Be-like
and F-like sequences to predict a large number of lines at UV and soft X-ray wavelengths.
July 2008 - CHIANTI v. 5.2.1 released!
The collisional data for Fe XIII were mistakenly taken from an older version
of the database and were different from the Gupta & Tayal data we had selected.
This affected the emissivities of a few Fe XIII lines. Version 5.2.1 corrects
them.
April 2006 - Ne VI missing transition added
The radiative decay of level 2 to the ground level in Ne VI
has been added to the ne_6.wgfa file. This change has no effect in solar
coronal plasmas, but it makes a difference for lower density plasmas.
March 2006 - CHIANTI v. 5.2 released!
A few collisional transitions were mistakenly left out of the fe_17.splups file, that caused
the emissivities of a few lines to be incorrectly calculated at densities larger than 10^12 cm^-3.
Also, the collisional excitation rate for the 5-11 transition in O IV was also mistakenly left out,
affecting the emissivity of this line at densities larger than 3x10^8 cm^-3. These transitions are
now included in CHIANTI.
The CHIANTI continuum IDL routines have also been modified to include the keyword
/keV that allows the calculation of the continuum emission
photon/cm^2/s/sr/keV (or erg/cm^2/s/sr/keV)
September 2005 - CHIANTI v. 5.1 released!
CHIANTI V. 5.1 corrects for an error in the Fe dielectronic satellite lines in the
1.7-2.0 Angstrom range, and a few software bugs affecting isothermal calculations
and the two-photon continuum.
August 2005 - CHIANTI v. 5 released!
We would like to announce the release of the version 5.0 of the CHIANTI database for astrophysical
spectroscopy. With Version 5, CHIANTI includes ionization and recombination as mechanisms for
populating excited levels, photoexcitation from any user-defined radiation field, software for
taking into account non-Maxwellian velocity distributions, and new data for a large number of ions
(both for new entries or for ions already in the database).
Changes in the data consist of the inclusion of high-energy configurations of Fe XVII to XXIII
to predict a large number of lines in the X-rays, n=3 configurations in the N-like
and O-like sequences to predict a large number of lines at UV wavelengths, and new data for
very important ions in the EUV wavelength range such as Fe IX, Fe XII and Fe XV.
The software has been speeded considerably and a few more user-friendly features have been added.
Atomic Data Updates
The updates contained in Version 4.0 of CHIANTI involve ions emitting at all wavelength
ranges. Updates by iso-electronic sequence are as follows:
- Hydrogen sequence
- He II, Ne X, Na XI, Mg XII, P XV, Cl XVII, K XIX
- Helium sequence
- He I, C V, N VI, O VII, Ne IX, Na X, Mg XI, Al XII, Si XIII, P XIV, S XV, Cl XVI, Ar XVII, K XVIII, Ca XIX, Fe XXV
- Lithium sequence
- Fe XXIV
- Beryllium sequence
- C III, O V, Ar XV, Fe XXIII
- Boron sequence
- C II, N III, O IV, Ne VI, S XII, Ar XIV, Fe XXII
- Carbon sequence
- O III, Ne V, S XI, Cl XII, Fe XXI
- Nitrogen sequence
- Mg VI, S X, Cl XI, Ar XII, Ca XIV, Fe XX
I, Zn XXIV
- Oxygen sequence
- Ne III, Mg V, Al VI, Si VII, P VIII, S IX, Cl X, Al XI, K XII, Ca XIII, Ti XV, Cr XVII, Mn XVIII,
Fe XIX, Co XX, Ni XXI, Zn XXIII
- Fluorine sequence
- Fe XVIII
- Neon sequence
- Ar IX, Fe XVII
- Magnesium sequence
- Al II, Fe XV
- Aluminum sequence
- S IV, Ca VIII
- Silicon sequence
- Ca VII, Fe XIII
- Phosphorus sequence
- K V, Fe XII
- Sulphur sequence
- Cl II
- Argon sequence
- Fe IX
- Potassium sequence
- Fe VIII
- Calcium sequence
- Fe VII
CHIANTI IDL Procedures Updates
- Software
- Routines speeded up considerably
- New software for photoexcitation from user-defined radiation fields
- New software for non-Maxwellian velocity distributions
December 3, 2003 - CHIANTI v 4.2 released!
Version 4.2 corrects a few errors in the following files:
- O II : o_2.splups
- N VI : n_6.splups
- C V : c_5.splups
- S II : s_2.wgfa
- Si II : si_2.wgfa
- Ne III : ne_3.wgfa
- Al XII : al_12.wgfa
- Fe XIX : fe_19.wgfa, fe_19.splups
- Fe XXIIId : fe_23d.elvlc, fe_23d.wgfa
and improves the wavelengths and energy level values for the following ions:
- Ca XVIIId : ca_18d.wgfa
- Fe XX : fe_20.wgfa, fe_20.elvlc
- Fe XXIId : fe_22d.wgfa
- Fe XXIVd : fe_24d.wgfa
- Fe XXIV : fe_24.elvlc, fe_24.wgfa
- Fe XXVd : fe_25d.wgfa
New data for two innershell transitions for Fe XXIII have been inserted: they
have been calculated using the Flexible Atomic Code developed by Dr. Ming-Feng Gu.
Moreover, collisional data for some missing transitions from metastable levels were
inserted for the following ions: Ar IV, Fe VIII, N I, Ne VII, Ni XIII and Ni XVI.
Details for these changes have been inserted in the comments of each modified file.
The software was corrected for an error that affected all the satellite lines in
the X-rays, a bug in the calculation of the freefree continuum, and a few minor bugs;
many improvements were also added, mostly for Windows-compatibility.
August 8, 2003 - CHIANTI software v 4.1 made available
We have corrected a few minor bugs and added a few improvements. See the HISTORY file for details.
February 6, 2003 - CHIANTI v. 4.02 released!
Since the release of CHIANTI 4.0 we have discovered errors in the ionization
equilibrium (.ioneq) files for the following ions:
- 1 - mazzotta_etal.ioneq, mazzotta_etal_ext.ioneq: Ar XII to Ar XIX
- 2 - arnaud_raymond.ioneq, arnaud_raymond_ext.ioneq: Fe VII
- 3 - shull_steenberg.ioneq, shull_steenberg_ext.ioneq: All Fe ions
Moreover, errors in the original papers were found for the ion fractions of
Ca I and Fe I (Arnaud & Rothenflug 1985).
December 2, 2002 - CHIANTI v. 4.01 released!
Since the release of CHIANTI 4.0 we have discovered errors in
two data files in CHIANTI:
- 1 - the "itoh.dat" file was corrupted
- 2 - the file "si_9.splups" was missing the 3-4 transition
The itoh.dat file is used in the calculation of the bremsstrahlung
continuum radiation. The missing 3-4 transition in Si IX affected
significantly the emissivities of only a few lines in the visible
and of the 258.08 A and 227.36 A lines in the EUV. Corrected versions
of both these files are now distributed in Version 4.01.
In order to improve backward-compatability, we also have included
in Version 4.01 the ion fractions, element abundances and DEM files
from Version 3 in the "version_3" subdirectories within the "ioneq/",
"abund/" and "dem/" directories.
September 2002 - CHIANTI v. 4 released!
We would like to announce the release of the Version 4.0 of the CHIANTI
database for astrophysical spectroscopy. With Version 4, CHIANTI includes
proton excitation rates for most of the ions in the database. New ions have
been inserted, expecially the first neutral species (H I, He I, N I), and data
for many ions have been renewed. Two-photon continuum radiation has been
included, along with a new code for calculating relativistic free-free
continuum. A new feature of the CHIANTI database is the use of 9-point spline
fitting to scaled effective collision strengths, that allows a more accurate
representation of upsilons over large temperature range.
We have completely rewritten the entire software and made it compatible with
Windows NT and VMS. The new software is compatible with the previous versions
of the database.
Atomic Data Updates
The updates contained in Version 4.0 of CHIANTI involve ions emitting at all wavelength
ranges. Updates by iso-electronic sequence are as follows:
- Updates by iso-electronic sequence are as follows:
- Hydrogen sequence
- H I
- Helium sequence
- He I
- Lithium sequence
- C IV, O VI
- Beryllium sequence
- O V, Al X, Si XI, S XIII, Ar XV, Ca XVII, Fe XXIII
- Boron sequence
- Al IX, Si X, S XII, Ar XIV, Ca XVI, Fe XXII
- Carbon sequence
- Ne V, Fe XXI
- Nitrogen sequence
- N I, O II, Mg VI, Al VII, Si VIII, P IX, S X, Ar XII, K XIII, Ca XIV, Ti XVI, Cr XVIII, Mn XIX, Fe XX, Co XXI, Ni XXII, Zn XXIV
- Oxygen sequence
- Ne III, S IX, Fe XIX, Ni XXI
- Fluorine sequence
- Fe XVIII
- Magnesium sequence
- Fe XV
- Phosphorus sequence
- S II, Ar IV, Fe XII
- Scandium sequence
- Fe VI
CHIANTI IDL Procedures Updates
- Software
- Completely rewritten
- Compatible with Windows NT and VMS
- Continuum
- Two-photon continuum added
- Free-free modified to include relativistic effects
- effective collision strengths fit
- 9-point spline fit added, to better reproduce effective collision strengths
Dec 20, 2001 - CHIANTI v. 3.03 of the database and software made available
It has recently been pointed out that the CHIANTI (x+y+z)/w intensity ratio of O VII and Si XIII in
the X-ray wavelength range were in disagreement with observations. Disagreements for O VII were moderate,
those for Si XIII were significant. We have discovered a small mistake in the transition energies of
transitions 1-5 and 1-6 in the o_7.splups and si_13.splups files which was the cause of these
disagreements. For this reason, the o_7.splups and si_13.splups files have been corrected (CHIANTI
version 3.03 of the database). We have also corrected a minor error in the 'freefree.pro' routine for
the calculation of the free free continuum. (CHIANTI version 3.03 of the software).
Nov 19 2001 - CHIANTI v. 3.02 of the software made available
We have discovered an error in the calculation of the free-free
continuum in the CHIANTI software package ('freefree.pro'). The error
was associated with the mislabeling of the original data file for the
gaunt factor. The effects of this error are significant only at high
temperatures, where the freefree contribution is most important.
The relevant procedures have been corrected and the whole software
package has been released as v. 3.02.
Apr 30 2001 - CHIANTI v. 3.02 of the database made available
It has recently been pointed out that the intensities of a few O V
lines predicted by the CHIANTI database are in disagreement with
SOHO/SUMER observations on the Sun. The collision rates in the
current (3.01) version of CHIANTI are from distorted wave calculations
from Zhang & Sampson 1992. However, their rates for O V do not appear
to agree well with the other members of the iso-electronic sequence.
It has been found that collisional transition proabilities from
Berrington et al. (1985) provide a better reproduction of the observations.
For this reason, the o_5.splups in the latest version of the CHIANTI
database (version 3.01) has been replaced with the Berrington et al.
(1985) data. The tar files on our web sites have been updated, as
Version 3.02. The only change from version 3.01 is the revised O V
collisional data. Also the files in the SolarSoft package have been updated
with the new data.
Some tests have shown that changes in the emissivities of the O V lines
in the EUV spectral range between 600 A and 800 A are moderate (within 10%),
while the effects on the 1218/1371 line ratio are greater. Electron densities
measured using the 1218/1371 line ratio are now much more in agreement with
estimates from ratios of other ions.
28 November 2000 - new CHIANTI package within SolarSoft made available
We have
reorganised and updated the whole CHIANTI package under SolarSoft:
$SSW/packages/chianti/
Now:
$SSW/packages/chianti/dbase/ contains the lite version 3.01 of the CHIANTI database
$SSW/packages/chianti/doc/ contains various documentation including
new software notes
In particular,
$SSW/packages/chianti/doc/chianti_guide_1.0.ps
replaces the previous CDS software notes #33,37,50 (now obsolete).
$SSW/packages/chianti/idl/ contains all the CHIANTI routines.
In particular, it contains the routines that before could only be found in
$SSW/soho/cds/idl/sci/data_anal/spec_syn
Also,
$SSW/packages/chianti/idl/extra/ contains some extra routines that Peter Young
contributed. These routines are described in the
$SSW/packages/chianti/doc/cds_swnote_52.ps document.
28 November 2000 - CHIANTI v. 3.01 of the procedures made available
We have updated some of the CHIANTI IDL routines.
The main changes affect the way the continuum was calculated.
Also, some minor bugs have been fixed.
We have also reorganised the routines into subdirectories,
so you will need to add to your IDL_STARTUP file (if not there
already):
!PATH = '+/data/chianti_pro_v3.01:'+!PATH
!PATH = EXPAND_PATH(!PATH)
The modified routines are:
temperature_ratios, gofnt, setup_ion, conf2n,
freebound,freefree,synthetic,synthetic_plot,
density_ratios, read_ioneq, latex_wvl_dem,
ascii_wvl_dem.
28 September 2000 - CHIANTI v. 3.01 made available
Since our announcement of the release of Version 3.0 of the CHIANTI
database we have determined that there are errors in few of the files
in that release. The errors include incorrect collisonal data for the
He II 304 line and two-photon transitions that appear as spectral lines
in some of the helium sequence ions. These files have been corrected
and a new version, Version 3.01, is now available.
If you have downloaded Version 3.0, we highly recommend that you
replace it with Version 3.01.
We regret any inconvenience this has caused you.
1 September 2000 - release of the new CHIANTI v. 3.0
We would like to announce the release of Version 3.0 of the CHIANTI
database for astrophysical spectroscopy. This release extends CHIANTI
into the X-ray wavelength region between 1 and 50 Angstroms.
This has largely been accomplished by including the necessary atomic
data for the hydrogen- and helium-like isoelectronic sequences and
their satellites. In addition, the atomic data for a number of other
ions have also been updated and revised.
In order to include the satellite lines, it has been necessary to
modify the IDL procedures that calculate spectral lines intensities.
Consequently, it is necessary to download both the new data files and
the new set of IDL procedures.
The additions to the database are described in a paper `CHIANTI - an atomic database for emission
lines, IV - Extension to X-ray Wavelengths' by K.P. Dere, E. Landi,
P.R. Young, and G. Del Zanna, and has been submitted to the
Astrophysical Journal Supplement Series.
Atomic Data Updates
The updates contained in Version 3.0 of CHIANTI are primarily concerned
with extending its coverage to include the 1 - 50 Å wavelength
region. The inclusion of emission lines from the hydrogen and helium
isoelectronic sequences and their satellite line and improved models of
highly ionized iron (Fe) ions are the principal ingredients for
achieving this. Below, we list the newly included ions and the ions
which have been modified for improved X-ray coverage.
- Updates by iso-electronic sequence are as follows:
- Hydrogen sequence
- C VI, N VII, O VIII, Ne X, Na XI, Mg XII, Al XIII, Si XIV, S XVI, Ar XVIII, Ca XX, Fe XXVI, Ni XXVIII
- Helium sequence (including satellites to the hydrogen-like lines)
- C V, N VI, O VII, Ne IX, Na X, Mg XI, Al XII, Si XIII, S XV, Ar XVII, Ca XIX, Fe XXV, Ni XXVII
- Lithium sequence satellites to the helium-like lines
- C IV, N V, O VI, Ne VIII, Na IX, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Fe XXIV, Ni XXVI
- Lithium sequence with inner-shell excitations
- O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Fe XXIV, Ni XXV
- Other dielectronic satellites to helium-lines
- Fe XXI, Fe XXII, Fe XXIII
- Beryllium sequence
- Mg IX: R-matrix collision strengths included
- Nitrogen sequence
- Fe XX: R-matrix collision strengths withing the ground configuration
- Neon sequence
- Fe XVII: n=4 levels now included
- Ni XIX: n=4 levels now included
- Silicon sequence
- S III
- Fe XIII: R-matrix collision strengths included for some transitions
- Sulphur sequence
- Fe XI: R-matrix collision strengths included for some transitions
- Chlorine sequence
- Fe X: n=4 and n=5 levels included
CHIANTI IDL Procedures Updates
Procedures for calculating the continuum due to free-free
(bremsstrahlung) and free-bound (radiative recombination) are now
included. Their names are 'FREEFREE' and 'FREEBOUND', respectively. A
procedure ('RAD_LOSS') calculates the total radiative loss rate as a
function of temperature for specified set of abundances and/or
ionization equilibria.
One nice feature initiated in Version 1.03 is that by typing the
name of a procedure, while in IDL, it's correct calling sequence is
returned.
We have also renamed some of the utility procedures ('ch_...') so that
they don't conflict with IDL procedures distributed with the Solar
Soft-Tree.
12 April 1999 - CHIANTI version 2 now available
Version 2.0 is now available for downloading at the following site:
http://www.chiantidatabase.org/
Version 2.0 adds atomic data for many of the so called minor
ions, such as fluorine and potassium, not included in the first
version. Because the astrophysical abundances of these elements are
relatively low, only the strongest lines of these elements are
observed. The addition of the minor ions is an important step in our
goal to understand astrophsical spectra in detail. In addition,
Version 2.0 extends the beryllium-like sequence, updates some of the
data in Version 1, and provides an IDL procedure to calculate the
continuum.
1 March 1999 - CHIANTI Paper III published
Paper III of the CHIANTI series has been published in the Astronomy &
Astrophysics Supplement Series (Vol. 135, 339-346). This paper
describes the updates that will be contained in Version 2 of the
database.
We are still performing checks on the new data and routines contained
in Version 2, but it will be ready for release soon.
20 Feb 1998 - REVISED Ca XVI FILE
The ca_16.splups file has been revised. You can download this
new file below:
ca_16.splups.
18 June 1997 - CHIANTI PAPER II SUBMITTED
The second paper in the CHIANTI series has been submitted to
Astronomy and Astrophysics, and in it we perform a detailed comparison of
theoretical line intensities predicted from the CHIANTI atomic data with
the observed intensities contained in the SERTS-89 active region spectrum.
The paper has been later published in Astronomy & Astrophysics 329, 291-314.
29 April 1997 - VERSION 1.01 RELEASED
We have made the following changes to the CHIANTI data base that is now
released as version 1.01. Because of the number of changes and
correction, we suggest that the complete database should be downloaded
following the standard procedures in the README file. When the version
1.01 tar file is extracted, if will simply overwrite the existing
files. There is no need to remove the version 1.0 files.
Alternately, you could extract it into a new directory, make sure that
your procedures work and then delete the old version.
Changes/corrections to the database are:
- 1. Fe X
- The wavelength of transition 1-5 was corrected to 256.239
from 256.197
- 2. Beryllium sequence
- C III, N IV, O V, Si XI: Peter Young has recalculated the necessary
oscillator strength and A values for these ion and these file have been
replaced.
- For C III, N IV, O V, Si XI and for Al X, S XIII and Ar XV the A value
for the 1-4 (2s2p 3P1 - 2s2p 3P2) transition was missing and has been
inserted into the version 1.01 files. It begins to dominate the
transition probability to the ground level for high values of Z
begining at Z=8 (Mg XI).
- Relatively small errors in the collision strength files (.splups)
involving the first 10 energy levels have been corrected.
- 3. Boron sequence
- For Si X, the collision strength to energy level 5 has been corrected.
Thanks to Martin Laming for pointing this out.
- For Fe XXII and Ni XXIV, the A values for the 1-2 transitions have been
corrected by roughly an order of magnitude. The correct A values are
Fe XXII: 1.47e+4
Ni XXIV: 3.95e+4
- 4. Fe XX
- The wavelengths and gf and A values are now those from the NIST
database. In particular, some of the strong lines in the EUVE short
wave spectra are better matched with these data. Thanks to Rolf Mewe
for pointing this out.
- 5. Differential emission measures
- In the first release of CHIANTI, the differential emission measures
were defined such that:
Intensity = Integral ( G(T) DEM(T) dlnT )
The advantage of this definition was that it was possible to compare to
isothermal emission measures in a fairly direct fashion. However, the
more standard definition is:
Intensity = Integral ( G(T) DEM(T) dT )
and we have decided to revert to this latter definition. Accordingly,
all the of sample differential emission measures in !xuvtop/dem have
been converted to this definition and the IDL procedures have been
changed to perform the standard integration.
- 6. Ionization equilibria
- The ionization equilibria Arnaud and Raymond (1992) for iron are also
now included in the file 'arnaud_raymond.ioneq' in the standard
directory. The ionization equilibria for all other ions are also
included in this file but the values are taken from Arnaud and
Rothenflug (1985). Thanks to Jeremy Drake for help in producing this
file.
- 7. IDL procedures
- A procedure isothermal.pro, written by Jeff Newmark (GSFC) is now
included in our distribution of CHIANTI IDL procedures. It allows the
calculation of the emitted spectrum at a specified temperature or at
several specified temperatures. The density at each temperature can
also be specified.
- Because of the change in the treatment of differential emission measure
files, it is also necessary to download the latest compressed tar file
of the CHIANTI IDL procedures: CHIANTI_1.02_pro.tar.Z
- The most conventient way to download these files is to go to our web site:
http://www.chiantidatabase.org/
- Please let us know of any problems or difficulties. Also, we believe
that CHIANTI can now be run on VMS machines but needs to be tested.
CHIANTI can also be easily adapted to run on Windows machines (Joan
Schmelz, U. Memphis, has already demonstrated this) and we hope to have
this incorporated into the next release.
- 8. CHIANTI and the Solar Software Library
- CHIANTI is now included as part of the Solar Software Library. The
CHIANTI consortium maintains a set of data files and IDL procedures on
the web. We consider these
to be the 'official' CHIANTI files. The Solar Software Library obtains
copies of these files. The data files should be identical. There are
small but significant modifications to the IDL procedures. These
modifications mostly involve the use of IDL system variables by the
CHIANTI IDL procedures and the use of Unix system variables by the
Solar Software Library versions of these programs.
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