2011A&A...529A..92K


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST16:01:08

2011A&A...529A..92K - Astronomy and Astrophysics, volume 529A, 92-92 (2011/5-1)

The initial period function of late-type binary stars and its variation.

KROUPA P. and PETR-GOTZENS M.G.

Abstract (from CDS):

The variation in the period distribution function of late-type binaries is studied. It is shown that the Taurus-Auriga pre-main-sequence population and the main-sequence G dwarf sample do not stem from the same parent period distribution with better than 95 per cent confidence probability. The Lupus, Upper Scorpius A, and Taurus-Auriga populations are shown to be compatible with being drawn from the same initial period function (IPF), which is inconsistent with the main-sequence data. Two possible IPF forms are used to find parent distributions to various permutations of the available data, which include Upper Scorpius B (UScB), Chameleon, and Orion Nebula Cluster pre-main-sequence samples. All the pre-main-sequence samples studied here are consistent with the hypothesis that there exists a universal IPF that is modified by binary-star disruption if it forms in an embedded star cluster leading to a general decline of the observed period function with increasing period. The pre-main-sequence data admit a log-normal IPF similar to that arrived at by Duquennoy & Mayor (1991A&A...248..485D) for main-sequence stars, provided the binary fraction among pre-main-sequence stars is significantly higher. However, for consistency with proto-stellar data, the possibly universal IPF ought to be flat along the log-P or log-semi-major axis and must be similar to the K1 IPF form derived by means of inverse dynamical population synthesis, which has been shown to lead to the main-sequence period function if most stars form in typical embedded clusters.

Abstract Copyright:

Journal keyword(s): binaries: general - stars: formation - stars: late-type

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2908 0
2 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1180 1
3 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3309 0
4 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1906 1
5 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1432 1
6 NAME Cha Dark Cloud SFR 11 55 -78.0           ~ 527 1
7 NAME Lup Cloud SFR 16 03 -38.1           ~ 481 0
8 NAME Upper Sco Association As* 16 12 -23.4           ~ 959 1
9 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1078 1
10 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2929 0
11 NAME Upper Scorpius B As* ~ ~           ~ 12 0
12 NAME Upper Scorpius A As* ~ ~           ~ 16 0

    Equat.    Gal    SGal    Ecl

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2019.10.21-16:01:08

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