Constraints on star formation in NGC2264. (arXiv:2112.00743v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Parker_R/0/1/0/all/0/1">Richard J. Parker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schoettler_C/0/1/0/all/0/1">Christina Schoettler</a> (University of Sheffield, UK)
We quantify the spatial distribution of stars for two subclusters centred
around the massive/intermediate mass stars S Mon and IRS1/2 in the NGC2264
star-forming region. We find that both subclusters are have neither a
substructured, nor a centrally concentrated distribution according to the
Q-parameter. Neither subcluster displays mass segregation according to the
$Lambda_{rm MSR}$ ratio, but the most massive stars in IRS1/2 have higher
relative surface densities according to the $Sigma_{rm LDR}$ ratio. We then
compare these quantities to the results of N-body simulations to constrain the
initial conditions of NGC2264, which are consistent with having been dense
($tilde{rho} sim 10^4$M$_odot$pc$^{-3}$), highly substructured and
subvirial. These initial conditions were also derived from a separate analysis
of the runaway and walkaway stars in the region, and indicate that star-forming
regions within 1kpc of the Sun likely have a broad range of initial stellar
densities. In the case of NGC2264, its initial stellar density could have been
high enough to cause the destruction or truncation of protoplanetary discs and
fledgling planetary systems due to dynamical encounters between stars in the
early stages of its evolution.
We quantify the spatial distribution of stars for two subclusters centred
around the massive/intermediate mass stars S Mon and IRS1/2 in the NGC2264
star-forming region. We find that both subclusters are have neither a
substructured, nor a centrally concentrated distribution according to the
Q-parameter. Neither subcluster displays mass segregation according to the
$Lambda_{rm MSR}$ ratio, but the most massive stars in IRS1/2 have higher
relative surface densities according to the $Sigma_{rm LDR}$ ratio. We then
compare these quantities to the results of N-body simulations to constrain the
initial conditions of NGC2264, which are consistent with having been dense
($tilde{rho} sim 10^4$M$_odot$pc$^{-3}$), highly substructured and
subvirial. These initial conditions were also derived from a separate analysis
of the runaway and walkaway stars in the region, and indicate that star-forming
regions within 1kpc of the Sun likely have a broad range of initial stellar
densities. In the case of NGC2264, its initial stellar density could have been
high enough to cause the destruction or truncation of protoplanetary discs and
fledgling planetary systems due to dynamical encounters between stars in the
early stages of its evolution.
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