Slow rotation of white dwarfs and baryon stars

Papoyan, V. V.; Sedrakyan, D. M.; Chubaryan, Eh. V.

doi:10.1007/bf01004706

Cited by 1 publication

(8 citation statements)

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“…It is clear that for a given central density the value of the total mass is larger in the case of a rotating object than for a static body. This is in accordance with the physical expectations based upon other alternative studies [18][19][20][21][22]. A similar behavior takes place when we explore the mass as a function of the equatorial radius, as shown in Fig.…”

Section: An Example: White Dwarfssupporting

confidence: 92%

“…As one can see from the Table, indeed Ω test > Ω Kep and this results are in agreement with the ones in the literature [19][20][21][22]. It should be stressed that the Keplerian angular velocity allows one to estimate the maximum rotation rate (the minimum rotation period) and the maximum rotating mass of stars.…”

Section: The Mass-shedding Limit and Scaling Lawsupporting

confidence: 91%

“…We conclude that the results obtained from the numerical integration of the differential equations derived by using the approach proposed in this work are consistent with the physical expectations, when restricted to the region in which the formalism can be applied [19][20][21][22][27][28][29]. …”

Section: An Example: White Dwarfssupporting

confidence: 84%

“…Notice that in all the plots, the selected values for the central mass and the equatorial radius are in accordance with the expected values for white dwarfs. We conclude that the results obtained from the numerical integration of the differential equations derived by using the approach proposed in this work are consistent with the physical expectations, when restricted to the region in which the formalism can be applied [19][20][21][22][27][28][29].…”

Section: An Example: White Dwarfssupporting

confidence: 82%

“…If we express Ω Kep = λΩ test , then the value of multiplicative factor λ can be estimated from the above procedure and the results are shown in Table I. As one can see from the Table , indeed Ω test > Ω Kep and this results are in agreement with the ones in the literature [19][20][21][22]. It should be stressed that the Keplerian angular velocity allows one to estimate the maximum rotation rate (the minimum rotation period) and the maximum rotating mass of stars.…”

Section: The Mass-shedding Limit and Scaling Lawsupporting

confidence: 82%

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Hartle formalism for rotating Newtonian configurations

et al. 2016

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We apply the Hartle formalism to study equilibrium configurations in the framework of Newtonian gravity. This approach allows one to study in a simple manner the properties of the interior gravitational field in the case of static as well as stationary rotating stars in hydrostatic equilibrium. It is shown that the gravitational equilibrium conditions reduce to a system of ordinary differential equations which can be integrated numerically. We derive all the relevant equations up to the second order in the angular velocity. Moreover, we find explicitly the total mass, the moment of inertia, the quadrupole moment, the polar and equatorial radii, and the eccentricity of the rotating body. We also present the procedure to calculate the gravitational Love number. We test the formalism in the case of white dwarfs and show its compatibility with the known results in the literature.

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