2018A&A...612A..74K


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET19:58:11

2018A&A...612A..74K - Astronomy and Astrophysics, volume 612A, 74-74 (2018/4-1)

Evidence for feedback and stellar-dynamically regulated bursty star cluster formation: the case of the Orion Nebula Cluster.

KROUPA P., JERABKOVA T., DINNBIER F., BECCARI G. and YAN Z.

Abstract (from CDS):

A scenario for the formation of multiple co-eval populations separated in age by about 1Myr in very young clusters (VYCs, ages less than 10Myr) and with masses in the range 600-20000M is outlined. It rests upon a converging inflow of molecular gas building up a first population of pre-main sequence stars. The associated just-formed O stars ionise the inflow and suppress star formation in the embedded cluster. However, they typically eject each other out of the embedded cluster within 106yr, that is before the molecular cloud filament can be ionised entirely. The inflow of molecular gas can then resume forming a second population. This sequence of events can be repeated maximally over the life-time of the molecular cloud (about 10Myr), but is not likely to be possible in VYCs with mass <300M, because such populations are not likely to contain an O star. Stellar populations heavier than about 2000M are likely to have too many O stars for all of these to eject each other from the embedded cluster before they disperse their natal cloud. VYCs with masses in the range 600-2000M are likely to have such multi-age populations, while VYCs with masses in the range 2000-20000M can also be composed solely of co-eval, mono-age populations. More massive VYCs are not likely to host sub-populations with age differences of about 1Myr. This model is applied to the Orion Nebula Cluster (ONC), in which three well-separated pre-main sequences in the colour-magnitude diagram of the cluster have recently been discovered. The mass-inflow history is constrained using this model and the number of OB stars ejected from each population are estimated for verification using Gaia data. As a further consequence of the proposed model, the three runaway O star systems, AE Aur, µ Col and ι Ori, are considered as significant observational evidence for stellar-dynamical ejections of massive stars from the oldest population in the ONC. Evidence for stellar-dynamical ejections of massive stars in the currently forming population is also discussed.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - stars: luminosity function, mass function - HII regions - open clusters and associations: general - globular clusters: individual: ONC

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1182 1
2 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1182 1
3 HD 34078 Or* 05 16 18.1489437436 +34 18 44.347016027 5.48 6.18 5.96     O9.5V 515 1
4 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1907 1
5 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 991 2
6 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1256 1
7 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1433 1
8 * iot Ori SB* 05 35 25.9819073 -05 54 35.643537 1.45 2.53 2.77     O9IIIvar 723 0
9 NAME Ori A MoC 05 38 -07.1           ~ 2615 0
10 RMC 136 Cl* 05 38 42.396 -69 06 03.36   9.63 9.50     ~ 1676 2
11 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1058 1
12 * mu. Col V* 05 45 59.8953630749 -32 18 23.164726112 3.84 4.90 5.18 5.30 5.57 O9.5V 451 0
13 NGC 3603 HII 11 15 24 -61 15.0           ~ 922 2
14 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2938 0
15 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1857 1

    Equat.    Gal    SGal    Ecl

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2019.11.17-19:58:11

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