Rapidly Rotating Polytropes and Concave Hamburger Equilibrium
スポンサーリンク
概要
- 論文の詳細を見る
Rotating polytropes have equilibrium figures of concave hamburger shape, which bifurcates from Maclaurin-spheroid-like figures and continues into toroids. However, two existing numerical computations of the concave hamburgers are quantitatively in contradiction to each other. Reasons for this contradiction are found to lie in the wrong treatments: One of their methods was applied for deformations too strong to be treated within its limit of applicability so that their boundary condition failed in its convergence of the series and in its analytic continuation into the complex plane. A modified method of numerical computation is developed which can not only avoid such problems but is still reasonable efficient. With this method we have recomputed sequences of rotating polytropes. We have found the following. When the polytropic index N is greater than 0.02, the sequence of the Maclaurin-spheroid-like figures terminates by mass shedding from the equator. When N < 0.02, on the other hand, it continues into a sequence of the concave hamburgers. Contrary to the earlier computation, the Maclaurin spheroids are shown to be the limiting configuration to N=0. Some details are also discussed concerning the bifurcation to the concave hamburgers.
- 理論物理学刊行会の論文
- 1982-07-25
著者
-
HACHISU Izumi
Department of General Systems Studies, Graduate School of Arts and Sciences, The University of Tokyo
-
Hachisu Izumi
Department Of Aeronautical Engineering Kyoto University
-
SUGIMOTO Daiichiro
Department of Earth Science and Astronomy College of General Education, University of Tokyo
-
ERIGUCHI Yoshiharu
Department of Earth Science and Astronomy College of General Education, University of Tokyo
-
Sugimoto Daiichiro
Department Of Earth Science And Astronomy 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
-
Sugimoto Daiichiro
Department Of Earth Science And Astronomy College Of General Education University Of Tokyo
-
HACHISU Izumi
Department of Eaarth Sience 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
-
Sugimoto Daiichiro
Department of General Systems Studies, College of Arts and Sciences, The University of Tokyo
関連論文
- Photometric Observation and Numerical Simulation of Early Superhumps in BC Ursae Majoris during the 2003 Superoutburst
- Gravothermal Catastrophe of Finite Amplitude
- Gravothermal Catastrophe and Negative Specific Heat of Self-Gravitating Systems
- 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
- The Recurrent Nova U Scorpii in the 1999 Outburst : the First Detection of a Significant Orbital-Period Change
- 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
- Thermal Properties of Self-Gravitating Plane-Symmetric Configuration
- The PCI Interface for GRAPE Systems : PCI-HIB
- 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
- Evolution of the Stars
- Evolution of Carbon Stars. II : Carbon Burning Phase
- Evolution of Carbon Stars. I : Gravitational Contraction and Onset of Carbon Burning
- Advanced Phases of Evolution of Population II Stars : Growth of the Carbon Core and Shell Helium Flashes
- Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. I : General Treatment and Brief Summary of Results
- Evolution of a Star with Intermediate Mass after Hydrogen Burning
- Evolution of Population II Stars in the Helium-Burning Phase
- Concave Hamburger Equilibrium of Rotating Bodies
- Second Helium Flash and an Origin of Carbon Stars
- Helium Flash in Less Massive Stars
- An Energetics of Quasar