Evolution of rotating binary stars

Huang, Rongxia

doi:10.1051/0004-6361:20034041

Cited by 21 publications

(15 citation statements)

References 12 publications

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“…The other way is an effect arising from the redistribution of chemical elements due to the instabilities caused by rotation. This effect is much more important and it has been studied by many investigators (Endal & Sofia 1978;Pinsonneault et al 1989;Chaboyer & Zahn 1992;Zahn 1992;Meynet & Maeder 1997;Maeder 1997;Maeder & Zahn 1998;Maeder & Meynet 2000;Huang 2004aHuang , 2004b. The method of Kippenhahn & Thomas (1970) as modified by Meynet & Maeder (1997) is used in our model.…”

Section: Introductionmentioning

confidence: 99%

Angular momentum transport and element mixing in the stellar interior

Yang

2006

A&A

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Aims. The purpose of this work was to obtain diffusion coefficient for the magnetic angular momentum transport and material transport in a rotating solar model. Methods. We assumed that the transport of both angular momentum and chemical elements caused by magnetic fields could be treated as a diffusion process. Results. The diffusion coefficient depends on the stellar radius, angular velocity, and the configuration of magnetic fields. By using of this coefficient, it is found that our model becomes more consistent with the helioseismic results of total angular momentum, angular momentum density, and the rotation rate in a radiative region than the one without magnetic fields. Not only can the magnetic fields redistribute angular momentum efficiently, but they can also strengthen the coupling between the radiative and convective zones. As a result, the sharp gradient of the rotation rate is reduced at the bottom of the convective zone. The thickness of the layer of sharp radial change in the rotation rate is about 0.036 R in our model. Furthermore, the difference of the sound-speed square between the seismic Sun and the model is improved by mixing the material that is associated with angular momentum transport.

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Section: Introductionmentioning

confidence: 99%

Angular momentum transport and element mixing in the stellar interior

Yang

2006

A&A

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“…However, in the case with the effects of rotation and tide being considered, the components are triaxial ellipsoids. The condition for the mass overflow through Roche lobe flow should be revised as a 1 = r robe (Huang 2004b). It is assumed that the transferred mass is distributed within a thin shell at the surface of the primary before the transfer, and within a thin shell at the surface of the secondary after the transfer.…”

Section: Luminosity Accretionmentioning

confidence: 99%

“…The structure and evolution of rotating single stars has been studied by many investigators (Kippenhahn & Thomas 1970;Endal & Sofia 1976;Pinsonneaul et al 1989;Langer 1998Langer , 1999Huang 2004a). However, it is also very important to study the evolution of rotating binary stars (Jackson 1970;Chan & Chau 1979;Langer 2003;Huang 2004b;Petrovic et al 2005a,b;Yoon et al 2006). The effect of spin on structure equations has been investigated (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Burša (1989aBurša ( , 1988 took advantage of the high-order perturbing potential to describe rotational and tidal deformations to discuss the figures and dynamic parameters of synchronously orbiting satellites in the solar system. The equilibrium structure of the two components were treated as two nonsymmetric rotational ellipsoids with two different semi-major axes a 1 and a 2 (a 1 > a 2 ) by Huang (2004b). It is very important that Kippenhahn & Thomas (1970) introduced a method of simplifying the two-dimensional model with conservative rotation and allowed the structure equations for a one-dimensional star to incorporate the hydrostatic effect of rotation.…”

Section: Introductionmentioning

confidence: 99%

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Structure and evolution of rotationally and tidally distorted stars

Song

Zhong

Lü

2009

A&A

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Aims. This paper aims to study the configuration of two components caused by rotational and tidal distortions in the model of a binary system. Methods. The potentials of the two distorted components can be approximated to 2nd-degree harmonics. Furthermore, both the accretion luminosity (σ i ) and the irradiative luminosity are included in stellar structure equations. Results. The equilibrium structure of rotationally and tidally distorted star is exactly a triaxial ellipsoids. A formula describing the isobars is presented, and the rotational velocity and the gravitational acceleration at the primary surface simulated. The results show the distortion at the outer layers of the primary increases with temporal variation and system evolution. Besides, it was observed that the luminosity accretion is unstable, and the curve of the energy-generation rate fluctuates after the main sequence in rotation sequences. The luminosity in rotation sequences is slightly weaker than that in non-rotation sequences. As a result, the volume expands slowly. Polar ejection is intensified by the tidal effect. The ejection of an equatorial ring may be favoured by both the opacity effect and the g e (θ, ϕ)-effect in the binary system.

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“…In a rotating binary system, the joint effect of rotation and tides modifies the shapes of two components from the perfect sphere to triaxial ellipsoids (Landin et al 2009;Song et al 2009Song et al , 2011Huang 2004). Eggleton & Kiseleva (1998) have presented the equations governing the quadrupole tensor of a star distorted both by rotation and by the presence of a companion in a possibly eccentric orbit.…”

Section: Introductionmentioning

confidence: 99%

The structure of critically-rotating accreting stars

Song

Wang

Song

et al. 2017

A&A

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Context. The structure characteristics of the critically-rotating accretor in binaries are investigated in this paper, on the basis of the potential function including rotational and tidal distortions. Aims. Our aim is to investigate the structure of the accretor when the accreting star reaches the critical velocity. Methods. In this paper, we have implemented the prescription described by Kippenhahn & Thomas (1970, Proc. IAU Colloq., 4, 20) and Landin et al. (2009, A&A, 494, 209).Results. The traditional model merely included the hydrodynamical effect of rotation. When comparing this model with ours, we find that it is very necessary for the rapidly rotating accreting star to include the gravitational potentials from tides Ψ tide , and the distortions of the star resulting from rotation Ψ dis,rot . Furthermore, we find that the mean effective gravitational acceleration can be decreased in the distort model, and the star shifts towards low temperature and low luminosity. Rotation and tides can extend the convection zone below the surface, and reduce the convective core in the center of stars due to the Solberg-Hoiland criterion. Rotational distortions derived from Ψ dis,rot can intensify the critical velocity whereas the tide force derived from Ψ tide tends to reduce the critical velocity. Rapid rotation induced by mass transfer also causes the central temperature to decrease, and triggers efficient mixing which can significantly modify the H-profile.

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Evolution of rotating binary stars

Cited by 21 publications

References 12 publications

Angular momentum transport and element mixing in the stellar interior

Angular momentum transport and element mixing in the stellar interior

Structure and evolution of rotationally and tidally distorted stars

The structure of critically-rotating accreting stars

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