2008AJ....135.2380T


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.17CEST02:48:45

2008AJ....135.2380T - Astron. J., 135, 2380-2397 (2008/June-0)

"Tail-end" bondi-hoyle accretion in young star clusters: implications for disks, planets, and stars.

THROOP H.B. and BALLY J.

Abstract (from CDS):

Young stars orbiting in the gravitational potential well of forming star clusters pass through the cluster's dense molecular gas and can experience Bondi-Hoyle accretion from reservoirs outside their individual protostellar cloud cores. Accretion can occur for several million years after the stars form, but before the cluster disperses. This accretion is predominantly onto the disk and not the star. N-body simulations of stars orbiting in three young model clusters containing 30, 300, and 3000 stars are presented. The simulations include the gravitational potential of the molecular gas which smoothly disperses over time. The clusters have a star-formation efficiency of 33% and a radius of 0.22 pc. We find that the disks surrounding solar-mass stars in the N = 30 cluster accretes ∼0.01 M(1 minimum-mass solar nebula, MMSN) per Myr, with a 1σ width of 50 times due to variations in initial stellar positions and velocities within the cluster. The accretion rate scales as M 2.1±0.1 for stars of mass M. The accretion rate is ∼5 times lower for the N = 3000 cluster, due to its higher stellar velocities and higher temperature. The Bondi-Hoyle accretion rates onto the disks are several times lower than accretion rates observed directly onto young stars (e.g., Muzerolle et al. 2005): these two accretion rates follow the same M 2 behavior and may be related. The accreted disk mass is large enough that it may have a substantial and unappreciated effect on disk structure and the formation of planetary systems. We discuss a variety of implications of this process, including its effect on metallicity differences between cluster stars, compositional differences between a star and its disk, the formation of terrestrial and gas-giant planets, and isotopic anomalies observed in our solar system.

Abstract Copyright:

Journal keyword(s): ISM: kinematics and dynamics - planetary systems: formation - planetary systems: protoplanetary disks - solar system: formation - stars: formation

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1261 1
2 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1134 0
3 IC 348 OpC 03 44 34 +32 09.8           ~ 1255 1
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3694 0
5 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2057 1
6 NGC 1981 OpC 05 35 09 -04 25.9     4.2     ~ 76 0
7 NAME OMC 1S PoC 05 35 14.5 -05 25 49           ~ 71 1
8 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1509 1
9 M 42 HII 05 35 17.3 -05 23 28           ~ 3794 0
10 Ass Ori OB 1c As* 05 35 21 -05 20.5           ~ 129 1
11 NGC 1980 OpC 05 35 24 -05 54.9     2.5     ~ 93 0
12 NAME Ori A MoC 05 38 -07.1           ~ 2760 0
13 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 502 0
14 LDN 1641 MoC 05 39.0 -07 00           ~ 438 0
15 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1219 0
16 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1087 1
17 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 905 1
18 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1014 1
19 LDN 1689 DNe 16 32 22.5 -24 28 29           ~ 115 0
20 NAME Oph Cluster ClG 17 12 24.7 -23 21 01           ~ 248 0
21 Ass Ori OB 1a As* ~ ~           ~ 205 0

    Equat.    Gal    SGal    Ecl

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2021.05.17-02:48:45

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