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Spectroscopic data for ionized scandium
Spectroscopic data for scandium is sparse, while an extensive set is needed to introduce this element into stellar opacity calculations and, more importantly, into stellar... -
RhII oscillator strengths
This work reports oscillator strengths for transitions of astrophysical interest in singly ionized rhodium. Seventeen radiative lifetimes in Rh^+^ have been measured with the... -
Atomic data for X-ray lines of FeVIII and FeIX
The distorted wave extension of the autostructure code has been used to calculate energy levels, radiative transition probabilities and collisional excitation rates of Fe VIII... -
Effective collision strength of Ni XVII
Electron-impact excitation collision strengths are required for the analysis and interpretation of stellar observations. This calculation aims to provide effective collision... -
FeII forbidden lines radiative transition rates
We report electric quadrupole and magnetic dipole transitions among the levels belonging to 3d^6^4s, 3d^7^ and 3d^5^4s^2^ configurations of Fe II in a large scale configuration... -
ZnI atomic data
We present our calculated data including energy levels of 235 bound terms, oscillator strength gf-values of E1 transitions between these bound states and photoionization cross... -
Low-charge ions charge transfer rate coeff.
We present total and final-state resolved charge transfer (CT) rate coefficients for low-charge Ge, Se, Br, Kr, Rb, and Xe ions reacting with neutral hydrogen over the... -
Sulphur ions iso-electronic sequence
We present our calculated data including energy levels, radiative decay rates and effective collision strengths for all the transitions among fine-structure levels of n=3 or 4... -
Atomic Data for Neutron-Capture Elements. II
We present multi-configuration Breit-Pauli distorted-wave photoionization (PI) cross sections and radiative recombination (RR) and dielectronic recombination (DR) rate... -
Nebular NII lines effective recombination coeff.
In nebular astrophysics, there has been a long-standing dichotomy in plasma diagnostics between abundance determinations using the traditional method based on collisionally... -
Photoionization cross sections of Selenium ions
We present multi-configuration Breit-Pauli AUTOSTRUCTURE calculations of distorted-wave photoionization (PI) cross sections, and total and partial final-state resolved radiative... -
Radiative losses in solar and stellar coronae
The radiative-loss function is an important ingredient in the physics of the solar corona, transition region and flares. We investigate the radiative losses due to the... -
Li-like iso-electronic sequence
We present our calculated data including energy levels, radiative decay rates and effective collision strengths for all the transitions among the 24 fine-structure valence... -
C abundances in G and K nearby stars
We present a determination of photospheric parameters and carbon abundances for a sample of 172 G and K dwarf, subgiant, and giant stars with and without detected planets in the... -
Electron-impact excitation of H-like ions
Accurate atomic data for the less abundance Fe-peak elements are required for use in X-ray astrophysical studies. We calculate high quality electron-impact excitation collision... -
Atomic data for Al ions
Radiative and Auger decay data have been calculated for modeling the K lines of the aluminium isonuclear sequence, from Al0 to Al11+. Level energies, transition wavelengths,... -
Effective collision strengths of CrII
Absorption or emission lines of Cr II are observed in a wide variety of astrophysical spectra and accurate atomic data are urgently needed to interpret these lines. Many of... -
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... -
Na-like iso-electronic sequence. II.
We present our calculated data including energy levels, radiative decay rates and effective collision strengths for all the transitions among the 209 fine-structure levels...
