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The interplay between stellar feedback and the ISM has been my major research topic. In particular, I am interested in the impact that stellar winds and supernova remnants have on their environments, specifically within massive molecular clouds where new star clusters are born. I am also interested on the evolution of shells and supershells. I have experience on semi-analytic methods and also on code development for high-performance computing , as briefly described below.
Evolution of supernova Remnants (SNRs)
Evolution of supernova Remnants (SNRs)
A semi-analytic approach was developed in order to study the full evolution of SNRs from the early ejecta-dominated (ED) phase up to the momentum conserving stage. The initial conditions of the ejecta affect only during the ED stage, which may be important for dust formation and destruction in young remnants. Our calculations allowed us to study the impact of the ambient gas density and to show that the typical SNR evolution change dramatically in high-density media with remnants avoiding entirely the Sedov-Taylor stage.
3D thin-shell approximation on supercomputers
3D thin-shell approximation on supercomputers
I developed an updated version of the Thin-shell approximation to study shells and supershells. For the case of supernova remnants, the ejecta was included in the calculations as well as radiative cooling. A parallel code was implemented by using the Message Passing Interface (MPI) standard, which allowed us to compute a large set of calculations on supercomputers.
The formation of Globular clusters
The formation of Globular clusters
Our numerical calculations were then used to study the stellar winds and supernovae feedback on the early evolution of Globular clusters (GCs). We showed that several important observational constraints are explained by the effect that stellar feedback had on the natal gas clouds. Indeed, the requirement of dilution with natal gas, the small iron spreads and the anti-correlation of first generation stars with the cluster mass (or enriched 2G mass, see the right panel), are all closely related constraints.
The 1G fraction as a function of the second generation(s) mass. Stars and diamonds are data on Galactic and Magellanic Clouds GCs while the solid lines show model results.
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