Contraction of a Protostar up to the Stage of Quasi-Static Equilibrium
スポンサーリンク
概要
- 論文の詳細を見る
- 理論物理学刊行会の論文
- 1965-03-25
著者
-
Hayashi Chushiro
Department Of Nuclear Science Kyoto University
-
Nakano Takenori
Department Of Nuclear Science Kyoto University
-
HAYASHI Chushiro
Department of Nuclear Science : Research Institute for Fundamental Physics Kyoto University : National Aeronautics and Space Administration
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
- 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
- Chapter 6 Effects of Magnetic Fields on Star Formation : Part II Formation Processes of Protostars : Origin of the Solar System
- Fundamental Processes in Star Formation
- Adiabatic Collapse of Rotating Gas Clouds
- Isothermal Collapse of Rotating Gas Clouds
- Thermal and Dynamical Evolution of Gas Clouds of Various Masses
- Fragmentation of a Cloud and the Mass Function of Stars in Galactic Clusters
- Helium Capturing Reactions in Stars
- Evolution of Carbon Stars. II : Carbon Burning Phase
- Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. II : 10, 10^2, 10^3 and 10^4 Solar Masses without Radiation Flow
- Contraction of a Protostar up to the Stage of Quasi-Static Equilibrium
- Chapter 13 Ionization State and Magnetic Fields in the Solar Nebula : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
- Rapid Contraction of a Protostar to the Stage of Quasi-Hydrostatic Equilibrium. I : The Case of One Solar Mass without Radiation Flow
- 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
- Internal Structure of Very Massive Stars
- Hamiltonian Formalism in Non-local Field Theories