Research interests

The Computational Astrochemistry Group is very multidisciplinary and moves from micro to macroscales. The main goal is to link the theoretical and computational aspects of chemistry and astrophysics, ranging from the small-scale effects in quantum systems to the application of the microphysics on large-scales. We work at the edge between chemistry and astrophysics, performing both computational simulations as well as quantum chemistry calculations of basics gas-grain interaction. We provide state-of- the-art models that allow a comparison and a better interpretation of the observational data, employing them to perform 3D hydrodynamical simulations of different environments. The main research interests are: astrochemistry; computational astrophysics; chemistry of low-metallicity star-forming regions, metal-poor stars, chemistry of the interstellar medium, and galaxy formation and evolution. We further work on the development and improvements of astrochemical networks, with particular emphasis on computational methods for networks reduction and chemical kinetics. We recently started to develop a new experiment to study cosmic dust and the proccesses occurring on their surfaces. Have a look at the CODE (Cosmic Dust Experiment) website.

From Bovino+2019

Deuterium Fractionation

An important step towards the understanding of the star formation process is identifying the initial phases of the collapse, and deuteration is the best proxy for this purpose. This requires to build accurate chemical networks including spin-state chemistry and isomers to be employed in hydrodynamical simulations of magnetized and turbulent collapsing filaments and cloud cores. We work on the development of reliable chemical models to accurately follow the effect of freeze-out, H2 ortho-to-para ratio, and cosmic-rays on the deuterium fractionation to explore its role as chemical clock of such environments. Post-processes of hydrodynamical simulations are used to compare with observational data.

From Redaelli+2021

APEX and ALMA observations

Together with our collaborators in Bologna and Munich we employ observational data from APEX and ALMA to probe the physical and chemical conditions of star-forming regions. In particular, we focus on deuterated tracers, which are thought to provide information about the physical timescale of the star-formation process. Our targets are sources in the early stages of the star-formation process. The main goal is to catch prestellar cores via unique tracers like oH2D+ and probe their masses to see if high-mass prestellar cores do exist and then disentangle between the different theoretical scenarios.

ISM and star formation in Galaxies

We explore here the chemistry of the ISM in galaxies, both at solar metallicity as well as in metal-poor environments. We focus on the role of CII and on the H2 chemistry. CII is known to be one of the most important coolant in the interstellar medium, and it is considered a powerful tracer for the star formation activity. In addition, it can provide useful insights on the reionization epoch. Cosmological hydrodynamical simulations of galaxies at different metallicities and redshifts, including a proper chemical model which can follow the [CII] evolution, are very important to probe the correlation between [CII] and the star formation rate, and to follow the transition between the different phases of the ISM. The star formation process in metal-poor galaxies and how this correlates with the molecular gas is not yet fully understood. ALMA observations have reported a very inefficient star formation process in this kind of galaxies. It is then very important to perform galaxy simulations which are able to follow the evolution of the molecular gas for different dust grains compositions/distributions, and compare the results with recent observations.

Astrochemistry Package Krome

KROME is a package which aims to provide microphysics and chemical networks to be included in hydrodynamical simulations of astrophysical objects. We also work in collaboration with Tommaso Grassi on development of different reduction methods for astrochemical networks, and codes to solve chemistry in different astrophysical problems (e.g. PATMO for planetary atmosphere, Lemongrab for 1D shocks etc.)

From Bovolenta+ 2025

Multi-binding energy chemistry

The binding energy of molecules on relevant ice mantles represents one of the largest uncertainty in the chemical modelling of star- and planet-forming regions. Accurate ab-initio calculations of the interaction between molecules and dust-grains are poor, and often performed with strong approximation (e.g. assuming a single water) or low-level of ab-initio methods. In collaboration with Stefan Vogt (Chemistry Department, UdeC) we started the ambitious project to build an accurate database of binding energies on relevant astrophysical surfaces with reliable quantum ab-initio methods. At the same time we are also developing a multi-binding energy approach for chemical models, motivated by the energy distributions found from our chemistry calculations.

Readapted from Esser+2019

The Cosmic Dust Experiment

We are developing an active nanoparticle mass spectrometer under ultra-high vacuum and cryogenic conditions, to re-create in lab the typical conditions of dark clouds. This involves the construction of a Paul trap, where an individual particle can be trapped via the application of a RF potential. Once trapped the particle can be characterized and its asbolute mass determined. Through the measurement of the mass-difference once a gas molecule is deposited on the particle, we can measure the binding enenergy in a typical temperature-programmed desorption experiment. See more details here.

Credits: NASA/JPL

Planetary Atmospheres

Within this project we built a 1D chemo-thermal model to study the atmosphere of an exomoon belonging to a free-floating planet. We make use of our private code PATMO.

Email

stefanobovino (at) astro-udec.cl
stefanobovino (at) udec.cl

Phone

+56 - 41 - 220 - 7248

Address

Departamento de Astronomía
Avenida Esteban Iturra s/n
Casilla 160-C
Room 222
Universidad de Concepción
Concepción, Chile