Internal Structure of Very Massive Stars
スポンサーリンク
概要
- 論文の詳細を見る
Some models are computed for very massive stars (M=46.8M⦿) consisting of four regions: (I) a homogeneous radiative envelope, (II) a semiconvective intermediate zone, (III) a radiative intermediate zone and (IV) a homogeneous convective core. The semiconvective intermediate zone is formed in the consequence of growing convective instability which is characteristic in very massive stars and the distribution of composition in this region is determined so as to maintain the convective neutrality taking account of the effect of the gradient of mean molecular weight. It is shown that the very massive stars evolve essentially in the same way as less massive stars in their early phase and the growing convective instability has little influence on the effective temperature and luminosity of stars.
- 理論物理学刊行会の論文
- 1961-12-25
著者
-
HAYASHI Chushiro
Department of Nuclear Science : Research Institute for Fundamental Physics Kyoto University : National Aeronautics and Space Administration
-
Sakashita S.
Department of Physics, Hokkaido University
関連論文
- Size Distribution of Grains Growing by Thermal Grain-Grain Collision
- The Gas Drag Effect on the Elliptic Motion of a Solid Body in the Primordial Solar Nebula
- Dissipation of the Primordial Terrestrial Atmosphere Due to lrradiation of the Solar Far-UV during T Tauri Stage
- Dissipation of the Primordial Terrestrial Atmosphere Due to irradiation of the Solar EUV
- Stellar Evolution toward Pre-Supernova Stage. II : Carbon and Oxygen Stars of 1.5Mxodoi and 2.6Mxodoi
- Effect of Electron Capture on the Temperature in Dense Stars
- Evolution of Iron Stars : Gravitational Contraction and the Decomposition of Iron
- Proton-Neutron Concentration Ratio in the Expanding Universe at the Stages preceding the Formation of the Elements
- Stellar Synthesis of the α-Particle Nuclei Heavier than Ne^
- Rapid Thermonuclear Reactions in Supernova Explosion
- Thermal and Dynamical Properties of a Protostar and Its Contraction to the Stage of Quasi-Static Equilibrium
- Central Temperature and Density of Stars in Gravitational Equilibrium
- Evolution of the Stars
- Formation of the Planets
- Collapse and Flare-up of Protostars
- Analytic Solutions for Equilibrium of Rotating Isothermal Clouds : One-Parameter Family of Axisymmetric and Conformal Configurations
- Adiabatic Collapse of Rotating Gas Clouds
- Isothermal Collapse of Rotating Gas Clouds
- Thermal and Dynamical Evolution of Gas Clouds of Various Masses
- Helium Capturing Reactions in Stars
- Evolution of Carbon Stars. II : Carbon Burning Phase
- Contraction of a Protostar up to the Stage of Quasi-Static Equilibrium
- Growth of Solid Particles in the Primordial Solar Nebula
- 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
- Stellar Evolution toward Pre-Supernova Stage. I : Carbon and Oxygen Stars of 5M_&odoi;, 10M_&odoi; and 30M_&odoi;
- Evolution of Massive Stars. II : Helium-Burning Stage
- Instability of a Gaseous Envelope Surrounding a Planetary Core and Formation of Giant Planets
- The Evolution of Massive Stars. I
- The Catalysis of Nuclear Fusion Reactions by μ^--Mesons
- Evolution of a Star with Intermediate Mass after Hydrogen Burning
- Formation of Light Nuclei in the Expanding Universe
- On the Origin of Planetary Nebulae
- Internal Structure of Very Massive Stars
- Hamiltonian Formalism in Non-local Field Theories