2018A&A...615A..65V


Query : 2018A&A...615A..65V

2018A&A...615A..65V - Astronomy and Astrophysics, volume 615A, 65-65 (2018/7-1)

Spin rates and spin evolution of O components in WR+O binaries.

VANBEVEREN D., MENNEKENS N., SHARA M.M. and MOFFAT A.F.J.

Abstract (from CDS):


Context. Despite 50 yr of extensive binary research, we must conclude that the Roche lobe overflow/mass transfer process that governs close binary evolution is still poorly understood.
Aims. It is the scope of the present paper to lift the edge of the veil by studying the spin-up and spin-down processes of the O-type components of WR+O binaries.
Methods. We critically analyzed the available observational data of rotation speeds of the O-type components in WR+O binaries. By combining a binary evolutionary code and a formalism that describes the effects of tides in massive stars with an envelope in radiative equilibrium, we computed the corresponding rotational velocities during the Roche lobe overflow of the progenitor binaries.
Results. In all the WR+O binaries studied, we find that the O-type stars were affected by accretion of matter during Roche lobe overflow (RLOF) of the progenitor. This means that common envelope evolution, which excludes any accretion onto the secondary O star, has not played an important role in explaining WR+O binaries. Moreover, although it is very likely that the O-type star progenitors were spun up by mass transfer, many ended the RLOF (and mass transfer) phase with a rotational velocity that is significantly smaller than the critical rotation speed. This may indicate that during the mass transfer phase there is a spin-down process that is of the same order, although significantly less, than that of the spin-up process. We propose a Spruit-Tayler type dynamo spin-down suggested in the past to explain the rotation speeds of the mass gainers in long-period Algols.

Abstract Copyright: © ESO 2018

Journal keyword(s): binaries: close - stars: rotation - stars: magnetic field

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 SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9854 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5994 1
3 HD 47129 SB* 06 37 24.0417003671 +06 08 07.376246443 5.23 6.11 6.06     O8I+O7.5III 373 0
4 * gam02 Vel WR* 08 09 31.95013 -47 20 11.7108 0.64 1.58 1.83 1.85 2.00 WC8+O7.5III-V 855 0
5 HD 90657 WR* 10 26 31.4088129340 -58 38 26.179161012 9.53 10.07 9.65 9.84   WN5+O4-6 150 0
6 MR 30 WR* 10 51 06.0017663106 -62 17 01.648960573   11.69 11.35 11.32   WC6+O7.5V 95 0
7 HD 94546 WR* 10 53 44.8196302 -59 30 46.694249 10.38 10.94 10.51 10.48   WN4+O8V 114 0
8 HD 97152 WR* 11 10 04.0798305535 -60 58 44.962711416 7.47 8.03 8.07 8.91   WC7+O7V 176 0
9 HD 311884 WR* 12 43 50.9989169468 -63 05 14.811840934 11.45 11.64 10.81 10.59   WN6+O5V 159 0
10 HD 152270 WR* 16 54 19.6991728950 -41 49 11.535393651 6.26 6.80 6.597 6.72 6.39 WC7+O5-8 289 0
11 HD 320102 WR* 17 36 53.6231930035 -34 02 36.780841955 11.51 11.60 10.72 10.65   WN4+O5/7V 87 0
12 HD 168206 WR* 18 19 07.3628284656 -11 37 59.165038875 9.65 9.88 9.10     WC8+O8/9III/V 290 1
13 HD 186943 WR* 19 46 15.9393000440 +28 16 19.074048808 9.86 10.50 10.23     WN3+O9.5V 179 1
14 HD 193576 WR* 20 19 32.4230196684 +38 43 53.958209968 8.15 8.53 8.00     WN5+O6II-V 688 0
15 MR 114 WR* 22 09 33.4427302357 +57 44 30.525316054 12.78 12.91 12.12     WN4+O5V 134 0
16 HD 214419 WR* 22 36 53.9549498582 +56 54 20.985957352 8.68 9.21 8.80     WN6o+O9Ib/II 364 1

    Equat.    Gal    SGal    Ecl

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2021.07.25-17:28:29

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