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 Physics , 1996, DOI: 10.1103/PhysRevD.54.4944 Abstract: We present a formalism to obtain equilibrium configurations of uniformly rotating fluid in the second post-Newtonian approximation of general relativity. In our formalism, we need to solve 29 Poisson equations, but their source terms decrease rapidly enough at the external region of the matter(i.e., at worst $O(r^{-4})$). Hence these Poisson equations can be solved accurately as the boundary value problem using standard numerical methods.This formalism will be useful to obtain nonaxisymmetric uniformly rotating equilibrium configurations such as synchronized binary neutron stars just before merging and the Jacobi ellipsoid.
 Physics , 2012, DOI: 10.1142/S0218301311040177 Abstract: The properties of uniformly rotating white dwarfs are analyzed within the framework of general relativity. Hartle's formalism is applied to construct self-consistently the internal and external solutions to the Einstein equations. The mass, the radius, the moment of inertia and quadrupole moment of rotating white dwarfs have been calculated as a function of both the central density and rotation period of the star. The maximum mass of rotating white dwarfs for stable configurations has been obtained.
 Physics , 2008, DOI: 10.1111/j.1365-2966.2008.14122.x Abstract: A Roche model for describing uniformly rotating rings is presented and the results are compared with numerical solutions to the full problem for polytropic rings. In the thin ring limit, the surfaces of constant pressure including the surface of the ring itself are given in analytic terms, even in the mass-shedding case.
 Physics , 2008, Abstract: In this paper, we describe an analytical method for treating uniformly rotating homogeneous rings without a central body in Newtonian gravity. We employ series expansions about the thin ring limit and use the fact that in this limit the cross-section of the ring tends to a circle. The coefficients can in principle be determined up to an arbitrary order. Results are presented here to the 20th order and compared with numerical results.
 Physics , 2005, DOI: 10.1103/PhysRevD.72.024019 Abstract: Highly accurate numerical solutions to the problem of Black Holes surrounded by uniformly rotating rings in axially symmetric, stationary spacetimes are presented. The numerical methods developed to handle the problem are discussed in some detail. Related Newtonian problems are described and numerical results provided, which show that configurations can reach an inner mass-shedding limit as the mass of the central object increases. Exemplary results for the full relativistic problem for rings of constant density are given and the deformation of the event horizon due to the presence of the ring is demonstrated. Finally, we provide an example of a system for which the angular momentum of the central Black Hole divided by the square of its mass exceeds one.
 Physics , 2012, DOI: 10.1088/0004-637X/762/2/117 Abstract: The properties of uniformly rotating white dwarfs (RWDs) are analyzed within the framework of general relativity. Hartle's formalism is applied to construct the internal and external solutions to the Einstein equations. The WD matter is described by the relativistic Feynman-Metropolis-Teller equation of state which generalizes the Salpeter's one by taking into account the finite size of the nuclei, the Coulomb interactions as well as electroweak equilibrium in a self-consistent relativistic fashion. The mass $M$, radius $R$, angular momentum $J$, eccentricity $\epsilon$, and quadrupole moment $Q$ of RWDs are calculated as a function of the central density $\rho_c$ and rotation angular velocity $\Omega$. We construct the region of stability of RWDs ($J$-$M$ plane) taking into account the mass-shedding limit, inverse $\beta$-decay instability, and the boundary established by the turning-points of constant $J$ sequences which separates stable from secularly unstable configurations. We found the minimum rotation periods $\sim 0.3$, 0.5, 0.7 and 2.2 seconds and maximum masses $\sim 1.500$, 1.474, 1.467, 1.202 $M_\odot$ for $^{4}$He, $^{12}$C, $^{16}$O, and $^{56}$Fe WDs respectively. By using the turning-point method we found that RWDs can indeed be axisymmetrically unstable and we give the range of WD parameters where it occurs. We also construct constant rest-mass evolution tracks of RWDs at fixed chemical composition and show that, by loosing angular momentum, sub-Chandrasekhar RWDs (mass smaller than maximum static one) can experience both spin-up and spin-down epochs depending on their initial mass and rotation period while, super-Chandrasekhar RWDs (mass larger than maximum static one), only spin-up.
 Physics , 2008, DOI: 10.1111/j.1365-2966.2008.13540.x Abstract: An iterative method is presented for solving the problem of a uniformly rotating, self-gravitating ring without a central body in Newtonian gravity by expanding about the thin ring limit. Using this method, a simple formula relating mass to the integrated pressure is derived to the leading order for a general equation of state. For polytropes with the index n=1, analytic coefficients of the iterative approach are determined up to the third order. Analogous coefficients are computed numerically for other polytropes. Our solutions are compared with those generated by highly accurate numerical methods to test their accuracy.
 Physics , 2010, DOI: 10.1111/j.1365-2966.2010.17241.x Abstract: In this paper uniformly rotating relativistic rings are investigated analytically utilizing two different approximations simultaneously: (1) an expansion about the thin ring limit (the cross-section is small compared with the size of the whole ring) (2) post-Newtonian expansions. The analytic results for rings are compared with numerical solutions.
 Eugen Radu Physics , 2005, Abstract: We review a number of results recently obtained in the area of constructing rotating solitons in a four dimensional asymptotically flat spacetime. Various models are examined, special attention being paid to the monopole-antimonopole and gauged skyrmion configurations, which have a nonvanishing total angular momentum. For all known examples of rotating solitons, the angular momentum is fixed by some conserved charge of the matter fields.
 T. Papakostas Physics , 2005, Abstract: A generalization of the notion of surfaces of revolution in the spaces of General Relativity is presented. We apply this definition to the case of Carter's family [A] of solutions and we study the Kerr's metric with respect the above mentioned foliation.
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