2015A&A...577A.117S


Query : 2015A&A...577A.117S

2015A&A...577A.117S - Astronomy and Astrophysics, volume 577A, 117-117 (2015/5-1)

Model computations of blue stragglers and W UMa-type stars in globular clusters.

STEPIEN K. and KIRAGA M.

Abstract (from CDS):

It was recently demonstrated that contact binaries occur in globular clusters (GCs) only immediately below turn-off point and in the region of blue straggler stars (BSs). In addition, observations indicate that at least a significant fraction of BSs in these clusters was formed by the binary mass-transfer mechanism. The aim of our present investigation is to obtain and analyze a set of evolutionary models of cool, close detached binaries with a low metal abundance, which are characteristic of GC. We computed the evolution of 975 models of initially detached, cool close binaries with different initial parameters. The models include mass exchange between components as well as mass and angular momentum loss due to the magnetized winds for very low-metallicity binaries with Z = 0.001. The models are interpreted in the context of existing data on contact binary and blue straggler members of GCs. The models are based on our recently developed code for evolutionary modeling of cool close and contact binaries. The model parameters agree well with the observed positions of the GC contact binaries in the Hertzsprung-Russell diagram, and we achieve detailed parameters of several individual contact and near-contact binaries. Contact binaries in the lower part of the cluster main sequence are absent because there are no binaries with initial orbital periods shorter than 1.5d. Contact binaries end their evolution as mergers that appear in the BS region. Binary-formed BSs populate the whole observed BS region in a GC, but a gap is visible between low-mass mergers that are concentrated along the zero-age main sequence and binary BSs occupying the red part of the BS region. Very few binary mergers are expected to rotate rapidly and/or possess chemical peculiarities resulting from the exposure of the layers processed by CNO nuclear reactions. All other binary mergers are indistinguishable from the collisionally formed mergers. The results show that binary-formed BSs may constitute at least a substantial fraction of all BSs in a GC.

Abstract Copyright:

Journal keyword(s): binaries: close - stars: evolution - stars: low-mass - blue stragglers - globular clusters: general - binaries: eclipsing

Simbad objects: 26

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Number of rows : 26
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20     4.09     ~ 3912 0
2 Cl* NGC 104 WSB V7 EB* 00 26 08.8627905552 -72 07 01.483751964     15.844 16.032 15.482 ~ 24 0
3 NGC 188 OpC 00 47 11.5 +85 14 38           ~ 922 0
4 NGC 362 GlC 01 03 14.26 -70 50 55.6     6.58     ~ 1083 0
5 Cl Melotte 25 OpC 04 29 47.3 +16 56 53           ~ 3074 0
6 H88 11 Cl* 04 52 20 -68 59.5           ~ 16 0
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17422 0
8 NGC 2632 OpC 08 40 13.0 +19 37 16           ~ 1564 0
9 NGC 2682 OpC 08 51 23.0 +11 48 50           ~ 2342 0
10 NGC 5139 GlC 13 26 47.28 -47 28 46.1           ~ 3423 0
11 NGC 5139 5876 EB* 13 27 19.3263531240 -47 21 52.624401372   16.231 16.020 15.799 15.624 ~ 25 0
12 Cl* NGC 5466 SAW V28 EB* 14 05 24.64 +28 31 59.0   19.04 18.635   18.419 ~ 22 0
13 NGC 5466 GlC 14 05 27.29 +28 32 04.0     9.70     ~ 828 0
14 Cl* NGC 5466 SAW V29 EB* 14 05 29.00 +28 31 13.4   19.278 19.218   18.935 ~ 21 0
15 Cl* NGC 5466 SAW V30 BS* 14 05 35.05 +28 31 19.8   18.854 18.739   18.607 ~ 14 0
16 Cl* NGC 6121 SAW V66 EB* 16 23 25.5423829536 -26 29 11.800992372 17.98 17.77 16.93 16.37 15.77 ~ 15 0
17 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1847 0
18 Cl* NGC 6121 SAW V72 EB* 16 23 38.4880359196 -26 32 10.911560523 16.76 16.46 15.83 15.40 15.01 ~ 27 0
19 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1974 0
20 Cl* NGC 6397 RB V1 V* 17 40 55.9 -53 42 42           ~ 4 1
21 NGC 6541 GlC 18 08 02.36 -43 42 53.6           ~ 377 0
22 Cl* NGC 6809 SAW V60 SX* 19 39 57.71 -30 57 46.4   17.42 17.11     ~ 8 0
23 M 55 GlC 19 39 59.71 -30 57 53.1     6.49     ~ 852 0
24 [LLY2012] CMHO 239 EmO 19 41 44.18 +23 18 19.2           ~ 1 0
25 M 30 GlC 21 40 22.12 -23 10 47.5     7.10     ~ 1048 0
26 V* SX Phe SX* 23 46 32.8928138474 -41 34 54.769886474   7.54 7.31     A3V 341 0

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