Influence of Rotation on Stellar Evolution

Palacios, A.

doi:10.1051/eas/1362007

Cited by 18 publications

(17 citation statements)

References 111 publications

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“…However, all star are rotating and some of them possess magnetic fields, thus, the problem is 2D (or 3D, if magnetic-field effects are considered). For a physical description of effects of rotation on stellar evolution, see [406, 561]. Realistic models with rotation should account for deviation from spherical symmetry, modification of gravity due to centrifugal force, variation of radiative flux with local effective gravity, transfer of angular momentum and transport of chemical species.…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

462

382

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

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Section: Introductionmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

462

382

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“…In particular, it induces meridional circulations, as well as shear and baroclinic instabilities, which contribute to the redistribution of angular momentum and to the mixing of chemical elements (see for instance Talon 2008;Maeder 2009;Mathis 2013;Palacios 2013, for comprehensive reviews). Except for the Sun, the observational constraints remained sparse until the advent of the space-borne missions CoRoT (Baglin et al 2006a,b;Michel et al 2008) and Kepler (Borucki et al 2010;Bedding et al 2010;Chaplin et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Angular momentum redistribution by mixed modes in evolved low-mass stars

Belkacem

Marques

Goupil

et al. 2015

A&A

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Seismic observations by the space-borne mission Kepler have shown that the core of red giant stars slows down while evolving, requiring an efficient physical mechanism to extract angular momentum from the inner layers. Current stellar evolution codes fail to reproduce the observed rotation rates by several orders of magnitude and instead predict a drastic spin-up of red giant cores. New efficient mechanisms of angular momentum transport are thus required. In this framework, our aim is to investigate the possibility that mixed modes extract angular momentum from the inner radiative regions of evolved low-mass stars. To this end, we consider the transformed Eulerian mean (TEM) formalism, which allows us to consider the combined effect of both the wave momentum flux in the mean angular momentum equation and the wave heat flux in the mean entropy equation as well as their interplay with the meridional circulation. In radiative layers of evolved low-mass stars, the quasi-adiabatic approximation, the limit of slow rotation, and the asymptotic regime can be applied for mixed modes and enable us to establish a prescription for the wave fluxes in the mean equations. The formalism is finally applied to a 1.3 M benchmark model, representative of observed CoRoT and Kepler oscillating evolved stars. We show that the influence of the wave heat flux on the mean angular momentum is not negligible and that the overall effect of mixed modes is to extract angular momentum from the innermost region of the star. A quantitative and accurate estimate requires realistic values of mode amplitudes. This is provided in a companion paper.

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“…This makes the treatment of rotation in stellar evolution modelling very complex (e.g., Maeder et al, 2013;Mathis, 2013). Several books and reviews deal with the effect of rotation on stellar structure and evolution (see e.g., Tassoul, 2007;Maeder, 2009;Palacios, 2013;Goupil et al, 2014, and references therein). First of all, rotation breaks the spherical symmetry of stars and therefore creates a thermal imbalance.…”

Section: Rotationmentioning

confidence: 99%

“…The determination of an accurate expression for the IGW, AM flux F IGW is nowadays the object of intense theoretical research (see e.g., Talon, 2008;Palacios, 2013). …”

Section: Angular Momentum Transport and Rotational Mixing In Stellar mentioning

confidence: 99%

How accurate are stellar ages based on stellar models?

Lebreton

Goupil

Montalbán

2014

EAS Publications Series

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Abstract. Among the various methods used to age-date stars, methods based on stellar model predictions are widely used, for nearly all kind of stars in large ranges of masses, chemical compositions and evolutionary stages. The precision and accuracy on the age determination depend on both the precision and number of observational constraints, and on our ability to correctly describe the stellar interior and evolution. The imperfect input physics of stellar models as well as the uncertainties on the initial chemical composition of stars are responsible for uncertainties in the age determination. We present an overview of the calculation of stellar models and discuss the impact on age of their numerous inputs.

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Influence of Rotation on Stellar Evolution

Cited by 18 publications

References 111 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

Angular momentum redistribution by mixed modes in evolved low-mass stars

How accurate are stellar ages based on stellar models?

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