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Zr II & III electron-impact broadening parameters
The electron-impact widths for 30 Zr III lines were calculated using the modified semi-empirical (MSE) method. For two Zr II and four Zr III astrophysically important UV lines,... -
IRON Project. XLVII. Ni III
This paper reports R-matrix calculations of electron impact excitation rates for Ni III. The calculation includes 70 LS terms corresponding to the configurations 3d^8^, 3d^7^4s,... -
Fe XXIII fine structure level oscillator strengths
We tabulate theoretical line strengths, f-values and transition energies for the beryllium-like ion Fe XXIII. Transitions are between levels 2l_1_2l_2_S'L'J' and 2l_3_nl_4_SLJ... -
Ortho:para-H2 ratio in C and J shocks
Tables 2a-f and 4a-f contain an extensive set of parameters derived from our grid of C-type (tables 2a-f) and J-type (tables 4a-f) planar stationary shock models. Models of... -
Solar abundance of iron
Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the... -
Uncertainties in r-abundance distribution
Tables 1&2 correspond to the first estimate of the error factors affecting the {beta} decay rates of highly ionized heavy atoms in stellar environments. The uncertainties in... -
Fe II oscillator strengths
A sample of the agreement between experiment (recent experimental log(gf) values) and our method (orthogonal operator technique) is shown in table 1. The experimental data are... -
IRC+10216 Silicon and sulfur chemistry
We present a dynamical and chemical model of the inner wind of the carbon-rich, AGB star IRC+10216. We include the effect of pulsation-driven shocks on the gas envelope close to... -
16O18O isotopomer collision rate
In this paper, a chemical model of interstellar clouds including ^18^O and ^13^C isotopic reactions with a non-LTE calculations of ^16^O^18^O rotational population has been used... -
SiO production in interstellar shocks
We study the production of SiO in the gas phase of molecular outflows, through the sputtering of Si-bearing material in grains. The sputtering is driven by neutral particle... -
Infrared transitions of SiO
Spectroscopic properties of SiO have been calculated from highly correlated wave functions. The computed dipole moments for v=0-3 agree well with the experimental data of... -
C_2_ Phillips and CN Red bands in HD 56126
We present the detection of molecular absorption lines in the optical spectrum of the post-AGB star HD 56126. The C_2_ Phillips A^1^{PI}u-X^1^{SIGMA}^+^g(1,0), (2,0), and (3,0);... -
IRON Project VII. FeII radiative transitions
Table ls.dat contains all LS terms considered in this work and their energy values with complete designation. Table aij.dat contains f-, S-, and A-values of transitions, both in... -
IRON project VI. FeII collision strengths
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Stark broadening of CaIII
We have determined matrix elements for all experimental configurations of CaIII, including the 3s^3^p^6^3d configuration. These values have been obtained using intermediate... -
On the atomic constants of TaI
Cross sections for the excitation of transitions in the tantalum atom (Z=73) not related to the ground state have been measured using extended crossed beams and optical... -
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... -
Slow collisions of O6+ with H cross section
The electron capture in collisions of highly charged O6^+^ ions with ground state hydrogen atom is a very important process in the solar wind X-ray studies. In the present... -
Line list
Blue metal-poor stars (BMPs) are main sequence stars that appear bluer and more luminous than normal turnoff stars. They were originally singled out by using B-V and U-B colour... -
Mg-like ions energy levels
Multiconfiguration Dirac-Hartree-Fock (MCDHF) calculations and relativistic configuration interaction (RCI) calculations were performed for states of the 3l3l', 3l4l' and 3s5l...
