2013A&A...559A..38P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST21:36:18

2013A&A...559A..38P - Astronomy and Astrophysics, volume 559A, 38-38 (2013/11-1)

The expansion of massive young star clusters - observation meets theory.

PFALZNER S. and KACZMAREK T.

Abstract (from CDS):

Most stars form as part of a star cluster. The most massive clusters in the Milky Way exist in two groups - loose and compact clusters - with significantly different sizes at the end of the star formation process. After their formation, both types of clusters expand up to a factor 10-20 within the first 20Myr of their development. Gas expulsion at the end of the star formation process is usually regarded as the only possible process that can lead to such an expansion during this early period of development. We investigate the effect of gas expulsion by a direct comparison between numerical models and observed clusters and concentrate on clusters with masses >103M. For these clusters the initial conditions before gas expulsion, the characteristic cluster development, its dependence on cluster mass, and the star formation efficiency (SFE) are investigated. We performed N-body simulations of the cluster expansion process after gas expulsion and compared the results with observations. We find that the expansion processes of the observed loose and compact massive clusters are driven by completely different physical processes. As expected, the expansion of loose massive clusters is largely driven by the gas loss due to the low SFE of ∼30%. One new revelation is that all the observed massive clusters of this group seem to have a very similar size of 1-3pc at the onset of expansion. It is demonstrated that compact clusters have a much higher effective SFE of 60-70% and are as a result much less affected by gas expulsion. Their expansion is mainly driven by stellar ejections caused by interactions between the cluster members. The reason ejections are so efficient in driving cluster expansion is that they occur dominantly from the cluster centre and over an extended period of time. During the first 10 Myr the internal dynamics of loose and compact clusters thus differ fundamentally.

Abstract Copyright:

Journal keyword(s): galaxies: star clusters: general - stars: kinematics and dynamics - open clusters and associations: general

Simbad objects: 56

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Number of rows : 56

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 [T98b] 70 CGG 00 33 52.9 +07 15 02           ~ 6 0
2 HCG 7 CGG 00 39 15.9 +00 53 17   11.4       ~ 82 0
3 NAME VDB 0 OpC 00 40 29.385 +40 36 15.20 14.957 14.94 15.288 15.056 14.701 ~ 42 2
4 [NVK2008] KW249 Cl* 00 41 30.761 +40 58 01.09 20.862   19.136 18.356 17.406 ~ 6 0
5 [NVK2008] KW258 Cl* 00 41 33.384 +40 55 20.56 22.253   20.481 19.564 18.554 ~ 5 0
6 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10902 1
7 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
8 BSCG 1 SCG 00 56 -12.3           ~ 3 0
9 NGC 330 Cl* 00 56 20.59 -72 27 12.5 9.37 9.76 9.55   8.89 ~ 366 0
10 NGC 346 Cl* 00 59 05.090 -72 10 33.24           ~ 449 0
11 NGC 595 HII 01 33 33.53 +30 41 29.8           ~ 190 0
12 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
13 NGC 604 HII 01 34 32.1 +30 47 01           ~ 544 0
14 * chi Per * 02 18 04.5844857610 +57 30 58.757945030   7.036 6.0230     G7.0III 156 1
15 NGC 869 OpC 02 19 00 +57 07.7           ~ 426 0
16 IC 1805 OpC 02 32 42 +61 27.0   7.03 6.5     ~ 473 2
17 NGC 1818 GlC 05 04 13.300 -66 26 05.47   9.7       ~ 236 0
18 NGC 1847 Cl* 05 07 08.200 -68 58 15.49   12.508 12.469     ~ 86 0
19 NGC 1850 Cl* 05 08 50.190 -68 45 35.65   8.84 8.96     ~ 231 1
20 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
21 NGC 2004 Cl* 05 30 41.340 -67 17 21.83   9.6       ~ 262 0
22 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 235 0
23 Ass Ori OB 1c As* 05 35 21 -05 20.5           ~ 129 1
24 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
25 NGC 2157 Cl* 05 57 35.430 -69 11 48.67   10.35 10.16     ~ 118 0
26 NGC 2214 OpC 06 12 57 -68 15.6   11.04 10.93     ~ 118 0
27 NGC 2244 OpC 06 31 55 +04 56.5   5.26 4.8     ~ 563 4
28 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49   11.59 10.5     ~ 277 0
29 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 425 0
30 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 940 1
31 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 354 1
32 NAME Upper Sco Association As* 16 12 -23.4           ~ 1021 1
33 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 463 0
34 [DBS2003] 179 OpC 17 11 32.0 -39 10 38           ~ 33 0
35 Cl Trumpler 27 OpC 17 36 20 -33 31.0   8.24 6.7     ~ 90 1
36 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
37 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 629 0
38 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 443 0
39 [MFD2008] Stellar Cluster OpC 18 13 24.0 -17 53 31           ~ 12 0
40 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 935 2
41 [MCM2005b] 9 OpC 18 34 08 -09 14.0           ~ 13 0
42 RSGC 1 OpC 18 37 58 -06 53.0           ~ 86 0
43 Cl Stephenson 2 OpC 18 39 20 -06 01.7           ~ 82 0
44 Masgomas-1 Cl* 18 50 15.408 +00 20 58.07           ~ 5 0
45 [MCM2005b] 13 OpC 18 53 53 +00 37.7           ~ 8 0
46 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 779 0
47 NGC 6801 G 19 27 35.793 +54 22 22.46   14.8       ~ 32 0
48 [H25] IV HII 19 44 52.18 -14 51 58.1           ~ 11 0
49 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 790 0
50 NAME I Lac As* 22 41 +38.5           ~ 143 0
51 NGC 7380 OpC 22 47 21 +58 07.9   7.62 7.2     ~ 172 0
52 NGC 7419 OpC 22 54 20 +60 48.9     13.0     ~ 85 0
53 SH 2-152 HII 22 58 40.862 +58 46 59.27           ~ 131 1
54 Ass Ori OB 1a As* ~ ~           ~ 195 0
55 NAME Local Group GrG ~ ~           ~ 6970 0
56 NAME Cen-Crux As* ~ ~           ~ 24 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-21:36:18

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