30 Doradus, the double stellar birth scenario by $N$-body & textsc{warpfield} clouds. (arXiv:2205.06209v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dominguez_R/0/1/0/all/0/1">R. Dom&#xed;nguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pellegrini_E/0/1/0/all/0/1">Eric W. Pellegrini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">Ralf S. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahner_D/0/1/0/all/0/1">Daniel Rahner</a>

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 $M
approx 6.32times 10^4$ 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.

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 $M
approx 6.32times 10^4$ 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.

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