Electronic computations of astrophysical interest.

Oscillator Strengths of Astrophysical Interest

Identification of carbon forms in soot materials of astrophysical interest

We determined the carbon structures in condensed soot samples of variable C/H ratio by using both scanning and transmission electronmicroscopy.We identified several types of carbon structures. All the samples are formedmainly by “chainlike aggregates” of amorphous grains. A small amount of more ordered forms of carbon is also detected. A “poorly graphitized carbon” is formed on a pre-existing a...

Photodissociation of small carbonaceous molecules of astrophysical interest

Astronomical observations have shown that small carbonaceous molecules can persist in interstellar clouds exposed to intense ultraviolet radiation. Current astrochemical models lack quantitative information on photodissociation rates in order to interpret these data. We here present ab initio multi-reference configurationinteraction calculations of the vertical excitation energies, transition d...

Laboratory Synthesis of Molecular Hydrogen on Surfaces of Astrophysical Interest

We report on the first results of experiments to measure the recombination rate of hydrogen on surfaces of astrophysical interest. Our measurements give lower values for the recombination efficiency (sticking probability S x probability of recombination upon H-H encounter γ) than model-based estimates. We propose that our results can be reconciled with average estimates of the recombination rat...

Calculations of Nuclear Reactions of Astrophysical Interest Involving Unstable Nuclei

Nuclear reactions involving unstable nuclei play an important role in nucleosyn-thesis. Such reactions are mainly associated with explosive astrophysical scenarios occurring at the nal stages of stellar evolution. For many nuclear reactions involving unstable nuclei the direct reaction mechanism cannot be neglected and may even be the dominant reaction mechanism. For example, the direct{reactio...