2017A&A...600A.116V


Query : 2017A&A...600A.116V

2017A&A...600A.116V - Astronomy and Astrophysics, volume 600A, 116-116 (2017/4-1)

Investigating the rotational evolution of very low-mass stars and brown dwarfs in young clusters using Monte Carlo simulations.

VASCONCELOS M.J. and BOUVIER J.

Abstract (from CDS):

Context. Very low-mass (VLM) stars and brown dwarfs (BDs) present a different rotational behaviour from their solar mass counterparts.
Aims. We investigate the rotational evolution of young VLM stars and BDs using Monte Carlo simulations under the hypothesis of disk locking and stellar angular momentum conservation.
Methods. We built a set of objects with masses ranging from 0.01M to 0.4M and considered models with single- and double-peaked initial period distributions with and without disk locking. An object is considered to be diskless when its mass accretion rate is below a given threshold.
Results. Models with initial single-peaked period distributions reproduce the observations well given that BDs rotate faster than VLM stars. We observe a correlation between rotational period and mass when we relax the disk locking hypothesis, but with a shallower slope compared to some observational results. The angular momentum evolution of diskless stars is flatter than it is for stars with a disk which occurs because the moment of inertia of objects less massive than 0.2M remains pratically constant for a time scale that increases with decreasing stellar mass.
Conclusions. Comparing our results with the available observational data we see that disk locking is not as important in the low-mass regime and that the rotational behaviour of VLM stars and BDs is different from what is seen in their solar mass counterparts.

Abstract Copyright: © ESO, 2017

Journal keyword(s): methods: statistical - brown dwarfs - stars: low-mass - stars: pre-main sequence - stars: rotation - stars: rotation

Simbad objects: 16

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Number of rows : 16
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 NAME THA As* 00 00 -62.0           ~ 380 0
2 NGC 869 OpC 02 19 00 +57 07.7           ~ 441 0
3 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1271 1
4 IC 348 OpC 03 44 34 +32 09.8           ~ 1260 1
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3748 0
6 NAME 25 Ori Group OpC 05 24 36 +01 48.0           ~ 107 1
7 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2067 1
8 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 506 0
9 NGC 2264 OpC 06 40 58 +09 53.7           ~ 1635 0
10 NGC 2362 OpC 07 18 41 -24 57.3           ~ 367 0
11 NGC 2516 OpC 07 58 04 -60 45.2           ~ 615 0
12 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 332 0
13 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1023 1
14 NAME Upper Sco Association As* 16 12 -23.4           ~ 1115 1
15 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3200 1
16 NGC 6530 OpC 18 04 31 -24 21.5           ~ 365 0

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2021.08.04-15:13:42

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