• Stefano Bovino

    ASTROCHEMISTRY

  • Stefano Bovino

    QUANTUM CHEMISTRY

  • Stefano Bovino

    COMPUTATIONAL ASTROPHYSICS

WELCOME

ABOUT ME

Download my CV


Hi, I'm Stefano Bovino, DFG Postdoctoral Fellow at the Hamburg Observatory. Educated as a Quantum Chemist I joined the astrophysics community in 2012 when I started to work in the Computational Astrophysics group in Goettingen. I am an "Astrochemist". I currently work on the chemical modelling of the formation and evolution of different types of structures in the Universe, performing three-dimensional hydrodynamical simulations.
I co-develop and maintain the astrochemistry package KROME.

Education



2006-2008


University of Rome Sapienza
MSc. in Theoretical Chemistry.

2008


Harvard University
Short-term scholar with Prof. A. Dalgarno.

2008-2011


University of Rome Sapienza
PhD in Chemical Sciences.

RESEARCH EXPERIENCE



2011-2012


Cineca Supercomputing Center
ISCRA Postdoctoral Fellow.

2012-2015


Institute for Astrophysics, Goettingen
Postdoctoral Research Assistant.

2015-Current


Hamburg Observatory
DFG Postdoctoral Fellow.

AWARDS



2009


CfA, Harvard University
SAO Visiting Student Award.

2010


CfA, Harvard University
SAO Visiting Student Award.

2015


Carla Roetti Medal

MY RESEARCH

The main goal of my research 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. My main research interests are: astrochemistry; development and maintenance of the astrochemistry package KROME; computational astrophysics; chemistry of low-metallicity star-forming regions, metal-poor stars, chemistry of the interstellar medium, galaxy formation and evolution.

ASTROCHEMISTRY


Krome development

KROME is a package which aims to provide microphysics and chemical networks to be included in hydrodynamical simulations of astrophysical objects.
Krome Website

Reactivity under extreme conditions

Rate coefficients are the bricks of chemical models. Inelastic and reactive processes can be computed via quantum methods. Many important rates for the early Universe and ISM are still unknown.

Chemical clocks

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 networks including spin-state chemistry and isomers to be employed in hydrodynamical simulations.

GALAXIES/ISM


[CII] signatures

[CII] is 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.

H2 in metal-poor galaxies

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.

METAL-POOR STARS


PopIII-PopII transition

The explosion of primordial stars enriched the medium by metals and dust which regulate the formation of the second generation of stars. Investigating how these were formed it is fundamental also to probe the primordial environment where the first generation of stars were born.





PUBLICATIONS

My Publications @ ADS

Contacts


Hamburg Observatory

Gojenbergsweg 112, Hamburg, Germany

Call: +49 40 42838-8468

Email: stefano.bovino(at)uni-hamburg.de