New molecular dataset for planet formation chemistry and modeling

Detailed astrochemical models are essential for interpreting observations of interstellar and circumstellar molecules because they allow important physical features of the gas and its evolutionary history to be derived (Williams and Cieza 2011). Advances in astrochemical models are linked to changes in astrochemical databases, as well as experimental and theoretical estimations of rate coefficients (see e.g. Öberg et al. 2021). The science community now need access to such molecular data, including preferred ones, for further modeling, and it is critical to our knowledge of the chemistry of planet formation. As a result, atomic and molecular datasets and databases (such as VAMDC) have become critical for constructing models and simulations (see Albert et al. 2021 and references therein). The analysis of the studied rates provides valuable information on the presence of species. As a result, it is critical to investigate not only radiative processes, but also concurrent processes involving molecular ions, such as dissociative recombination (Kamp et al., 2017). Our goal is to calculate, compare, and analyze cross sections and rate coefficients for molecular ions such as hydrogen and helium for a various model parameters. - FULL TEXT available in PDF.