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

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概要

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• The evolution of collapsing protostars of 0.05, 1 and 20Mxodoi is studied with computations which include radiative as well as convective energy flow, which has been entirely neglected in previous papers I and II. It is found that, when a shock wave which has been generated at the center reaches the outermost layers, the protostars flare up suddenly. The protostar of 1Mxodoi increases its luminosity from 50^<-4>Lxodoi to a peak value 60^3Lxodoi in a period of the order of 10 days. This peak value depends scarcely on the initial conditions. After the flare-up, a convective region grows inwards from the surface and the luminosity is kept at 10^3Lxodoi by convection until the star finally reaches a stage of wholly gravitational equilibrium. The luminosity at this stage is found to be very sensitive to the stellar mass, being 8Lxodoi and 50^4Lxodoi for the protostars of 0.05 and 20Mxodoi, respectively. These computed values of the luminosity are high enough to cover the observations of infrared objects.

• 理論物理学刊行会の論文
• 1970-04-25

著者

• HAYASHI Chushiro

  Department of Physics, Kyoto University

• Hayashi Chushiro

  Department Of Nuclear Science Kyoto University

• Narita Shinji

  Department of Electronic Engineering, Doshisha University

• Narita Shinji

  Department Of Physics Kyoto University

• NAKANO Takenori

  Research Institute for Fundamental Physics, Kyoto University

• Nakano Takenori

  Research Institute For Fundamental Physics Kyoto University : National Radio Astronomy Observatory

• Nakano Takenori

  Research Institute For Fundamental Physics Kyoto University

関連論文

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• Primordial Solar Nebula Embedded in Corona
• 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
• Chapter 5 Collapse and Fragmentation of Isothermal Clouds : Part II Formation Processes of Protostars : Origin of the Solar System
• Chapter 4 The Equilibrium and the Stability of Rotating Isothermal Clouds : Part II Formation Processes of Protostars : Origin of the Solar System
• Fragmentation of Isothermal Sheet-Like Clouds. II : Full Nonlinear Numerical Simulations
• Fragmentation of Isothermal Sheet-Like Clouds. I : Solutions of Linear and Second-Order Perturbations Equation
• Characteristics of Collapse of Rotating Isothermal Clouds : Astrophysics and Relatively
• 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
• The Radiative Energy Loss from the Shock Front
• Fully Three-Dimensional Hydrodynamical Collapse and Formation of Binary System
• 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
• 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

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