Thermal and Dynamical Evolution of Gas Clouds of Various Masses

スポンサーリンク

概要

• 論文の詳細を見る

• The evolution of gas clouds of masses, 10^4, 10^2, 1 and 10^<-2> Mxodoi, with the population I composition is investigated both for transparent and opaque stages by comparing the rates of cooling, heating, contraction and expansion. As heating and cooling processes in the transparent stage, we consider the thermal radiation from grains, the line-emission by H_2, C^+, Si^+, C and O including the effect of self-absorption, the ionization of atoms by interstellar star-light and cosmic-ray particles, and the absorption of star-light by grains. In the opaque stage cooling is due to the diffusion of thermal photons. The results show that in the transparent stage a cloud much greater than 10^<-2> Mxodoi contracts freely and cools down to about 10°K if its mean density is greater than a certain crit-ical value which depends on the mass of the cloud. In the opaque stage the cloud undergoes nearly adiabatic free-fall. On the other hand, if a cloud of mass nearly equal to or smaller than 1×10^<-2> Mxodoi is formed with a mean density greater than a certain critical value, it establishes immediately gravitational equilibrium and the subsequent evolution is the Kelvin contraction.

• 1969-10-25

著者

• Hayashi Chushiro

  Department Of Nuclear Science Kyoto University

• Nakano Takenori

  Research Institute For Fundamental Physics Kyoto University

• HATTORI Tsuguo

  Department of Physics, Kyoto University

• Hattori Tsuguo

  Department Of Physics 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
• 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
• 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
• Internal Structure of Very Massive Stars
• Hamiltonian Formalism in Non-local Field Theories

もっと見る 閉じる

スポンサーリンク