The stability of rotating baryon stars

Arutyunyan, G. G.; Sedrakyan, D. M.

doi:10.1007/bf01011361

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“…The pulsations and stability of oblate rotating white dwarfs have been studied by Vartanyan (1974), and the stability of rotating baryon stars by Arutynnyan & Sedrakyan (1974). The relation of adiabatic pulsations to con vective instability of uniformly rotating gaseous masses has been investigated by Kochhar & Trehan (1974) and of differentially rotating gaseous masses by Kochhar (1 974).…”

Section: Rotating Starsmentioning

confidence: 98%

Nonradial Oscillations of Stars: Theories and Observations

Cox¹

1976

Annu. Rev. Astron. Astrophys.

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This paper is primarily concerned with a review of more general kinds of stellar oscillations than the purely radial, spherically symmetric type that has been con sidered extensively in the literature [see e.g. Cox (l974a) fo r a recent review dealing primarily with this kind of oscillation; see also Zhevakin (1963) and Christy (1966)]. For a comprehensive review, covering both radial and nonradial oscillations, see Ledoux & Walraven (1958). For a review of nonradial stellar oscillations see, for example, Ledoux (1974). See also Cox (1975).The most general kinds of stellar oscillations are governed by at least nine equations: the mass equation, three momentum equations (for the three com ponents of force or acceleration), the energy equation, three flux equations, and Poisson's equation fo r the gravitational field. If fo rces other than gravitational, such as magnetic, are also present, then the above equations would of course have to be supplemented appropriately. Except where specified otherwise, however, we ignore these additional fo rces in this paper.To the best of the author's knowledge, the above set of nonlinear, partial differen tial equations has not been solved without significant approximations or special assumptions fo r any star or stellar system. (Various attempts are described in later sections.) In the case of spherical symmetry, Poisson's equation admits of a trivial solution, and the six momentum and t1ux equations reduce to two. The resulting system, normally of the third order in time and of the fo urth order in space (but still nonlinear), has by now been solved on fa st digital computers in a number of cases [see e.g. Cox (1974a) for recent references; see also Stellingwerf (1974Stellingwerf ( , 1975].In the case of small oscillations, but without any particular assumptions regarding symmetry, a linear theory is normally used, in which the Lagrangian or Eulerian variations, say (jP or P', respectively, are assumed "small" compared with the "unperturbed" values, say Poor P (for short), of the corresponding physical variables. In such a theory the angular dependence of the variations is usually assumed expressible in terms of spherical harmonics as described below. The radial depen-247 Annu. Rev. Astro. Astrophys. 1976.14:247-273. Downloaded from www.annualreviews.org by ILLINOIS STATE UNIVERSITY on 10/27/12. For personal use only.Quick links to online content Further ANNUAL REVIEWS

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Section: Rotating Starsmentioning

confidence: 98%

Nonradial Oscillations of Stars: Theories and Observations

Cox¹

1976

Annu. Rev. Astron. Astrophys.

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The stability of rotating baryon stars

Cited by 1 publication

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Nonradial Oscillations of Stars: Theories and Observations

Nonradial Oscillations of Stars: Theories and Observations

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