CHIANTI: What's new in Version 3.0?

We would like to announce the release of Version 3.0 of the CHIANTI database for astrophysical spectroscopy. This now extends the database to include the 1 - 50 Å wavelength region. 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, G. Del Zanna, and P.R. Young and has been submitted to the Astrophysical Journal Supplement Series. The new material is described below.

The best way to access CHIANTI is through our WWW page:

http://wwwsolar.nrl.navy.mil/chianti.html

*** PLEASE NOTE ***

If you already have a previous version of CHIANTI, it is necessary to download both the new data files and the new set of IDL procedures to run Version 3. In order to include dielectronic satellite lines, it has been necessary to modify our general procedures for calculating line intensities. Consequently, the new data set is not compatible with the old procedures and vice versa.

Also, if you use the Solar Softree, it is possible that the IDL routines distributed by the Solar Softree have not been immediately updated and there is the possibility of interference between the old routines and the new Version 3 routines now available at the CHIANTI web page.

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

Carbon sequence

N II, O III, Ne V, Na VI, Mg VII: transition probabilities updated

Fe XXI: atomic model now includes n=4 and n=5 levels

Oxygen sequence

Ne III, Na IV, Mg V: transition probabilities updated

Neon sequence

Ar IX, Ca XI, Fe XVII and Ni XIX: n=4 levels now included

Aluminum sequence

Si II: radiative data updated

S IV: radiative data updated and collision strengths to n=4 included

Fe XIV: radiative and collisional data updated

Silicon sequence

S III: radiative and collisional data updated

Fe XIII: R-matrix collision strengths included for most transitions

Sulphur sequence

Fe XI: R-matrix collision strengths within the ground configuration included

Chlorine sequence

Fe X: n=4 and n=5 levels included

Calcium sequence

Fe VIII: major update of radiative and collisional data

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 rename some of the utility procedures ('ch_...') so that they don't conflict with IDL procedures distributed with the Solar Soft-Tree.

If you find any problems, please let us know.

Return to CHIANTI Home Page