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IRON Project XXIX. Boron isoelectronic sequence
As part of the IRON Project, radiative rates have been calculated for the E1, E2 and M1 transitions within the n=2 complex in ions of the boron isoelectronic sequence... -
IRON Project XXXI. Fe XII electron excitation
The following tables list energy levels and electron excitation data for the lowest 41 levels of Fe XII (configurations 3s^2^ 3p^3, 3s 3p^4^ and 3s^2 ^3p^2^ 3d). The table... -
Stark broadening of Sc X & XI, Ti XI & XII
By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Sc X, 10 Sc XI, 4 Ti XI and 27 Ti XII... -
Stark broadening of O VII and Mg XI
Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 14 O VII and 18 Mg XI multiplets. For O VII,... -
Einstein A-Coefficients in SiC2 transitions
Einstein A-coefficients for the electric dipole transitions in Silicon Dicarbide molecule and its isotopomers between rotational levels of the ground vibrational state up to... -
Modeling the Mg I from the NUV to MIR. II.
We present a new atomic model for MgI that that encompasses and improves upon the model presented in Peralta et al. (2022A&A...657A.108P) for the Sun. We test our model on... -
Partially accreted crusts of neutron stars
Neutron stars in low-mass binary systems are subject to accretion when material originating from the companion star accumulates on the surface. In most cases, the justified and... -
BSk26 functionals
In the cooling process of a non-accreting neutron star, the composition and properties of the crust are thought to be fixed at the finite temperature where nuclear reactions... -
Spectroscopy of CH2(CN)2 and CNCH2CN
Nitriles constitute almost 20% of the molecules observed in the interstellar medium, whereas only one dinitrile and one isocyanonitrile compound have been detected up to now.... -
SII, ClII, ArIV energy levels & transition data
The aim of this work is to present accurate and extensive results of energy spectra and transition data for the SII, ClIII, and ArIV ions. These data are useful for... -
Thermodynamic quantities of molecular hydrogen
Hydrogen is the most abundant molecule in the Universe. Its thermodynamic quantities dominate the physical conditions in molecular clouds, protoplanetary disks, etc. It is also... -
GaIV, GaV, and GaVI oscillator strengths
For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are... -
Si XI K-shell energy levels and radiative rates
Atomic data for K-shell transitions are essential for modeling the K absorption lines, which have been observed in the spectra of active galaxies by high-resolution X-ray... -
Trans-HCOOH hyperfine structure
Formic acid, HCOOH, is the simplest organic acid and the first that has been identified in the interstellar medium. Its astrophysical relevance has motivated this spectroscopic... -
S V effective collision strengths
Effective collision strengths are presented in this table for all the transitions among the 26 fine-structure levels arising from the 14 lowest LS states of S V, i.e. those with... -
Rotational excitation of CS
The present paper focuses on the calculation of new rate coefficients among the 31 first rotational levels of the CS molecule in collision with He for temperatures ranging from... -
Fe XVI radiative and excitation rates
In this paper we report calculations for energy levels, radiative rates, collision strengths, and effective collision strengths for transitions in Fe XVI. For energy levels and... -
Cd III Stark broadening parameters
Stark broadening parameters, widths and shifts, for 84 spectral lines of doubly-ionized cadmium (Cd III) have been calculated using the modified semi-empirical approach (MSE).... -
Diatomic molecules collisional rates
A number of diatomic molecules have been found in vibrationally excited states in several cosmic objects. The molecules in vibrationally excited states provide valuable... -
Einstein A-coefficients for C_3_H_4_
Following tentative detection of cyclopropene (C_3_H_4_) in Sgr B2 through its transition 3_22_-2_21_, several attempts to confirm the presence of cyclopropene in astronomical...
