Giant Stars with Shell Sources of C-N and p-p Reactions
スポンサーリンク
概要
- 論文の詳細を見る
Structures of giant stars of population II producing energy in the C-N shell source are studied taking account of the contribution of the ion pressure in the partially degenerate isothermal core and also of the exact fitting of the radiative region to the convective one. Further, it is found that pure hydrogen stars producing energy in the p-p shell source can also explain the giant branch of population II if the effect of the ion pressure is included in the core.
- 理論物理学刊行会の論文
著者
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
- Giant Stars with Shell Sources of C-N and p-p Reactions
- Thermal and Dynamical Properties of a Protostar and Its Contraction to the Stage of Quasi-Static Equilibrium
- Proton-Neutron Concentration Ratio in the Expanding Universe at the Stages preceding the Formation of the Elements.
- Central Temperature and Density of Stars in Gravitational Equilibrium
- Evolution of the Stars
- Formation of the Planets
- Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III : Stars of 0.05, 1.0 and 20Mxodoi with Energy Flow by Radiation and Convection
- Collapse and Flare-up of Protostars
- Analytic Solutions for Equilibrium of Rotating Isothermal Clouds : One-Parameter Family of Axisymmetric and Conformal Configurations
- Advanced Phases of Evolution of Population II Stars : Growth of the Carbon Core and Shell Helium Flashes