On Some Effects in the Structure of White Dwarfs

Zhami, Bakytzhan; Boshkayev, Kuantay; Quevedo, Hernando; Kalymova, Zh. A.

doi:10.32014/2019.2518-1726.75

Cited by 1 publication

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References 18 publications

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“…From that moment this solution is widely known as the Hartle-Thorne (HT) solution. Unlike other solutions of the Einstein equations, the Hartle-Thorne solution has an internal counterpart [4,16], which makes it more practical for investigation the equilibrium structure and physical characteristics of relativistic compact objects such as white dwarfs, neutron stars and hypothetical quark stars [17][18][19][20][21]. Relatively recently this solution was extended up to Ω approximation [22].…”

Section: Introductionmentioning

confidence: 99%

To the Inverse Problem of Celestial Mechanics

Boshkayev¹,

Malybayev²,

Quevedo³

et al. 2021

SPM

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The link between exterior solutions to the Einstein gravitational field equations such as the exact Erez-Rosen metric and approximate Hartle-Thorne metric is established here for the static case in the limit of linear mass quadrupole moment (Q) and second order terms in total mass (M). To this end, the Geroch-Hansen multipole moments are calculated for the Erez-Rosen and Hartle-Thorne solutions in order to find the relationship among the parameters of both metrics. The coordinate transformations are sought in a general form with two unknown functions in the corresponding limit of ~Q and ~M^2. By employing the perturbation theory, the approximate Erez-Rosen metric is written in the same coordinates as the Hartle-Thorne metric. By equating the radial and azimuthal components of the metric tensor of both solutions the sought functions are found in a straightforward way. It is shown that the approximation ~Q and ~M^2, which is used throughout the article, is physical and suitable for solving most problems of celestial mechanics in post-Newtonian physics. This approximation does not require the use of the Zipoy-Voorhees transformation, which is a necessary strict mathematical requirement in the ~Q approximation, i.e. when no other approximations are made. This implies that the explicit form of the coordinate transformations depends entirely on the approximation that is adopted in each particular case. The results obtained here are in agreement with the previous results in the literature and can be applied to different astrophysical goals. The paper pursues not only pure scientific, but also academic purposes and can be used as an auxiliary and additional material to the special courses of general theory of relativity, celestial mechanics and relativistic astrophysics.

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