Rapidly Rotating and Fully General Relativistic Polytropes
スポンサーリンク
概要
- 論文の詳細を見る
A technique used in numerical computations of the Newtonian rotating polytropes has been generalized to compute general relativistic polytropes. Full equations for the rotating polytrope in general relativity have been numerically integrated without any approximation. The strength of relativity is measured μ≡p_c/ε_cc^2 where p_c,ε_c and c are the central pressure, the central energy density and the light velocity, respectively. Rotating sequences with μ=0.001 (almost Newtonian case), 0.25 (mildly relativistic case) and 0.5 ( highly relativistic case) have been obtained for the polytropic index N=1.5. The largest rotation in each sequence is so rapid that the surface velocity at the equator reaches about one-third of the light velocity for μ=0.25 and 0.5 cases.
- 理論物理学刊行会の論文
- 1980-12-25
著者
-
ERIGUCHI Yoshiharu
Department of Earth Science and Astronomy College of General Education, University of Tokyo
-
Eriguchi Yoshiharu
Department Of Earth Science And Astronomy University Of Tokyo
-
Eriguchi Yoshiharu
Department Of Earth Science And Astronomy College Of General Education University Of Tokyo
-
ERIGUCHI Yoshiharu
Department of Earth Science and Astronomy Graduate School of Arts and Science, University of Tokyo
関連論文
- Two Kinds of Axially Symmetric Equilibrium Sequences of Self-Gravitating and Rotating Incompressible Fluid : Two-Ring Sequence and Core-Ring Sequence
- Gravitational Equilibrium of a Multi-Body Fluid System
- Rapidly Rotating Polytropes and Concave Hamburger Equilibrium
- Dumb-Bell-Shape Equilibria and Mass-Shedding Pear-Shape of Selfgravitating Incompressible Fluid
- Gravothermal Aspects in Evolution of the Stars and the Universe
- New Equilibrium Sequences Bifurcating from Maclaurin Sequence
- Bifurcation and Fission of Three Dimensional, Rigidly Rotating and Self-Gravitating Polytropes
- Equation of Motion and a Possibility of Snapping of a Free Cosmic String Loop : Astrophysics and Relativity
- Darwin-Riemann Problems in Newtonian Gravity
- Stable Numerical Method in Computation of Stellar Evolution
- Another Equilibrium Sequence of Self-Gravitating and Rotating Incompressible Fluid
- Possible Evolutionary Transition from Rapidly Rotating Neutron Stars to Strange Stars Due to Spin-Down(Astrophysics and Relativity)
- Rapidly Rotating and Fully General Relativistic Polytropes
- Concave Hamburger Equilibrium of Rotating Bodies