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We study the evolution of embedded star clusters as possible progenitors to reproduce 30 Doradus, specifically the compact star cluster known as R136 and its surrounding stellar family, which is believed to be part of an earlier star formation event. We employ the high-precision stellar dynamics code NBODY6++GPU to calculate the dynamics of the stars embedded in different evolving molecular clouds modelled by the 1D cloud/clusters evolution code WARPFIELD. We explore clouds with initial masses of $M_\text{cloud}=3.16 \times 10^{5}$ M$_\odot$ that (re)-collapse allowing for the birth of a second generation of stars. We explore different star formation efficiencies in order to find the best set of parameters that can reproduce the observation measurements. Our best-fit models correspond to a first stellar generation with masses between $1.26 \times 10^4$ - $2.85 \times 10^4 $M$_\odot$ and for the second generation we find a $M \approx 6.32\times 10^4$ M$_\odot$. Our models can match the observed stellar ages, cloud shell radius, and the fact that the second generation of stars is more concentrated than the first one. This is found independently of the cluster starting initially with mass segregation or not. By comparing our results with recent observational measurements of the mass segregation and density profile of the central zone we find close agreement, and thus provide supporting evidence for a centrally focused (re)-collapse origin to the multiple ages., Comment: 13 pages, 7 figures, 2 tables

We study the evolution of embedded star clusters as possible progenitors to reproduce 30 Doradus, specifically the compact star cluster known as R136 and its surrounding stellar family, which is believed to be part of an earlier star formation event. We employ the high-precision stellar dynamics code NBODY6++GPU to calculate the dynamics of the stars embedded in different evolving molecular clouds modelled by the 1D cloud/clusters evolution code WARPFIELD. We explore clouds with initial masses of $M_\text{cloud}=3.16 \times 10^{5}$ M$_\odot$ that (re)-collapse allowing for the birth of a second generation of stars. We explore different star formation efficiencies in order to find the best set of parameters that can reproduce the observation measurements. Our best-fit models correspond to a first stellar generation with masses between $1.26 \times 10^4$ - $2.85 \times 10^4 $M$_\odot$ and for the second generation we find a $M \approx 6.32\times 10^4$ M$_\odot$. Our models can match the observed stellar ages, cloud shell radius, and the fact that the second generation of stars is more concentrated than the first one. This is found independently of the cluster starting initially with mass segregation or not. By comparing our results with recent observational measurements of the mass segregation and density profile of the central zone we find close agreement, and thus provide supporting evidence for a centrally focused (re)-collapse origin to the multiple ages., 13 pages, 7 figures, 2 tables

Stars and the gas between them - the interstellar medium - are intrinsically coupled. Massive stars form in clouds of molecular gas and illuminate them with their radiation, thus creating regions of ionized hydrogen (HII regions) and photodissociation regions. Eventually these stars destroy their parent clouds via powerful feedback mechanisms: stellar winds, ionizing radiation, and supernova explosions. These feedback processes are a crucial self-regulation mechanism of star formation, since, as soon as the first massive stars have formed, further star formation is suppressed. Stellar winds, radiation, and supernova feedback interact with each other in a highly non-linear manner. This complexity poses a problem not only for purely analytic approaches but also for three-dimensional hydrodynamical simulations due to the high computational cost. Here, I present a novel, semi-analytic, one-dimensional model, called WARPFIELD, which allows the cost-efficient simulation of the effects of stellar feedback from a massive star cluster on its natal giant molecular cloud (GMC). With WARPFIELD we can show that the strength of each feedback process depends strongly on time and environment. For a large range of GMC and star cluster properties we can also demonstrate that stellar feedback can naturally explain the observed inefficiency of star formation.