Chemical Evolution of Galaxies in their Cosmological Context

Research Interests

As a numerical astrophysicist, I have introduced the following mecanisms in the simulation code Gadget-2 :

Radiative Cooling :
- for a gas of primordial composition in photoionisation equilibrium, following Katz et al. (1996);
- with the contribution of molecular hydrogen transition lines, following Galli & Palla (1998);
- with the correction induced by atomic lines of heavy elements, using Sutherland & Dopita (1993) tables.
Heating by photoionisation :
- takes into account a UV background produced by QSO and Starburst galaxies (Haardt & Madau, 2001);
- include as well the local contribution from massive stars, by using Stromgren sphere around the sources.
Star Formation process :
a phenomenological approach offer the possibility to form simple stellar populations under particular conditions of the medium
Baryonic matter recycling :
stellar mass losses (stellar winds and SN ejecta) are return to the ISM according to the chosen IMF
Feedback by supernovae (SN) :
modeling Sedov explosions by the kinetic action of shell pistons
chemical enrichment of the ISM by heavy elements
Turbulent metallic diffusion :
transport of heavy elements along the gradients of concentration
AGN activity :
introduction of BH seeds
merging of close sink particles
baryonic disk accretion
kinetic jet feedback

Follow the link to see a collection of movies
that illustrate the impact of some of the above mecanisms