Star clusters do not form in isolation, but enshrouded in hierarchical gaseous filaments embedded in a galactic tidal field. To understand the role of radiation, stellar winds and supernovae of massive stars in regulating the multiphase interstellar medium we must decipher how the young host clusters form, evolve and interact with their surrounding galactic environment. In this talk, I present...
The GigaEris simulation is a cosmological, N-body hydrodynamical "zoom-in" simulation of the formation of a Milky Way-sized galaxy with the unprecedented resolution of better than a thousand solar masses, encompassing of order a billion particles within the refined region. The simulation employs a modern implementation of smoothed-particle hydrodynamics, including metal-line cooling and...
Stars will typically spend the first few million years of their lives in their natal star-forming regions. The initial densities in these regions often mean young stars are much more likely to experience the effects of close encounters, massive star stellar winds and potentially even nearby supernovae. Therefore, understanding the dynamical evolution of star-forming regions is key to...
To understand the impact of radiation feedback during the formation of a globular cluster (GC), we simulate a head-on collision of two turbulent giant molecular clouds (GMCs). A series of idealized radiation-hydrodynamic simulations is performed, with and without stellar radiation or Type II supernovae. We find that a gravitationally bound, compact star cluster of mass $M_{GC} \sim 10^5...
The formation of multiple populations of stars in globular clusters and their further evolution is still the subject of much debate and awaiting resolution. Many scenarios have been proposed to explain their formation. One of the most commonly proposed is the AGB scenario, in which chemically reprocessed gas from the envelopes of AGB stars mixes back with primary gas flowing into the center of...
Globular clusters (GCs) are among the most fascinating objects in the Universe, but their formation and evolution remain a key challenge in astrophysics. These dense and compact agglomerates of stars are believed to have formed from the dense cores of super-giant molecular clouds during the earliest stages of galaxy formation. However, the environment in which GCs originated is still quite...
Star clusters (SCs) are not born in spherical symmetry, contrary to the idealized initial conditions used in the vast majority of $N$-body simulations performed so far. Observations suggest that the initial conditions for star formation are highly structured and clumpy, both in the distribution of molecular gas from which stars form (Williams 1999 and references therein) and in the...
Initial conditions of stellar cluster simulations generally consist of a monolithic structure. However, both theoretical and observational studies suggest that stellar clusters form hierarchically and therefore host subclusters that could trigger stronger stellar interactions. Hence, it is fundamental to include more detailed initial conditions when studying the evolution of stellar clusters...
We have proposed a formation scenario for dSph galaxies which does not include any interaction with other galaxies, called the Dissolving Star Cluster Model. In this model the gas, accumulating inside the dark matter halo of the dwarf forms stars in form of small star clusters and associations which orbit the central region of the dark matter halo. These small entities do not survive for...
