Primordial Solar Nebula Embedded in Corona

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概要

• 論文の詳細を見る

• In order for the primordial solar nebula to be stable against fragmentation, Shakra-Sunyaev parameter a must be sufficiently large. We show in this article that the large value of a is derived naturally from the Hoiland instability.

著者

• Hayashi Chushiro

  Kyoto University

• Kiguchi Masayoshi

  近畿大学理工学総合研究所

• KIGUCHI Masayoshi

  Research Institute for Science and Technology, Kinki University

• NARITA Shinji

  Science and Engineering Research Institute, Doshisha University

• Narita Shinji

  Department of Electronic Engineering, Doshisha University

• Hayashi C

  Kyoto University

• Narita S

  Science And Engineering Research Institute Doshisha University

• Kiguchi M

  Kinki Univ. Higashi‐osaka Jpn

• NARITA Shinji

  Department of Electonics, Doshisha University

• KIGUCHI Masayoshi

  Research Institute for Science and Technology Kinki University

関連論文

• The Formation of Molecules in Contracting Interstellar Clouds
• Primordial Solar Nebula Embedded in Corona
• Morphology of Distant Galaxies
• Wind from T Tauri Stars
• The Structure and Evolution of Thin Viscous Disks-1-Non-steady Accretion and Excretion
• Chapter 23 Gas Capture by Proto-Jupiter and Proto-Saturn : Part VI Growth of the Planets : Origin of the Solar System
• 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
• The Radiative Energy Loss from the Shock Front
• Fully Three-Dimensional Hydrodynamical Collapse and Formation of Binary System
• Hydrogen Molecule Formation in the Collapsing Phase of Initial Cosmological Perturbation
• Hot Dense Matter and Stellar Collapse
• Note on Wind from T Tauri Stars〔和文〕
• An Attempt on the High Resolution Calculation by the Nested Grid Method
• Formation of first generation stars
• The Quantum Chromodynamic Black Body Radiation and the Universe
• Neutrino Cooling of Neutron Stars in Pion-Condensed Phase
• Excitation Energies in π-Electron Systems : Application of Green's Function Method with Second-Order Perturbaton Terms
• Characteristics of Collapse of Rotating Isothermal Clouds

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