Chapter 12 Settling of Dust Particles and Formation of Planetesimals : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
スポンサーリンク
概要
- 論文の詳細を見る
Dust particles which are initially distributed homogeneously in the solar nebula aggregate each other and settle toward the midplane. As a result, the solar nebula separates into three layers: a thin dust-gas layer(or, simply called the dust layer)around the midplane and two residual gas layers. As the settling proceeds, the density in the dust-gas layer increases, and finally, the dust-gas layer becomes gravitationally unstable and fragments into a number of planetesimals.
- 理論物理学刊行会の論文
- 1989-03-10
著者
-
Nakagawa Y
Department Of Earth And Planetary Sciences Faculty Of Science Kobe University
-
Nakagawa Yoshitsugu
Geophysical Institute University Of Tokyo
-
Nakagawa Yoshitsugu
Geophysical Institute Faculty Of Science University Of Tokyo
-
SEKIYA Minoru
Department of Applied Physics, Tokyo Institute of Technology
-
Sekiya Minoru
Department Of Earth And Planetary Sciences Faculty Of Sciences 33 Kyushu University
-
Sekiya Minoru
Department Of Applied Physics Tokyo Institute Of Technology
-
SEKIYA Makoto
Department of Physics, Kyoto University
-
SEKIYA Minoru
Department of Physics, Kyoto University
-
SEKIYA Minoru
Department of Earth and Planetary Sciences, Faculty of Sciences 33, Kyushu University
-
NAKAGAWA Yoshitsugu
Department of Physics, Kyoto University
関連論文
- Gas Drag on a Rotating Body with Gravity
- Chapter 12 Settling of Dust Particles and Formation of Planetesimals : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
- The Formation of Molecules in Contracting Interstellar Clouds
- Chapter 14 Dissipation of the Solar Nebula : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
- Origin of the Solar System : Planetary Growth in the Gaseous Nebula
- Chapter 16 Gravitational Scattering between Planetesimals and Their Statistical Behavior : Part V Physical Processes Relevant to the Planetary Growth : Origin of the Solar System
- Chapter 11 Cooling of the Solar Nebula : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
- Size Distribution of Grains Growing by Thermal Grain-Grain Collision
- Cosmic-ray exposure age and heliocentric distance of the parent body of H chondrites Yamato-75029 and Tsukuba
- Collisional destruction experiment of chondrules and formation of fragments in the solar nebula
- Formation processes of magnetic spherules collected from deep-sea sediments -Observations and numerical simulations of the orbital evolution-
- Chapter 20 Accumulation Process of Planetesimals to the Planets : Part VI Growth of the Planets : Origin of the Solar System
- Statistical Behavior of Planetesimals in the Primitive Solar System
- The Surface Wave Instability of Stratified Incompressible Cylinders with Differential Rotation : Astrophysics and Relativity
- Numerical Simulation of Viscous Flow by Smoothed Particle Hydrodynamics : Astrophysics and Relativity
- Were planetesimals formed by dust accretion in the 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
- Chapter 23 Gas Capture by Proto-Jupiter and Proto-Saturn : Part VI Growth of the Planets : Origin of the Solar System
- Flow in a Liquid Sphere Moving with a Hypersonic Velocity in a Rarefied Gas : An Analytic Solution of Linearized Equations
- Gravitational Instabilities in a Dust-Gas Layer and Formation of Planetesimals in the Solar Nebula
- Chapter 8 Efficiency of Angular Momentum Transfer by Shear Instability : Part II Formation Processes of Protostars : Origin of the Solar System
- Chapter 7 Stability of the Primordial Solar Nebula : Part II Formation Processes of Protostars : Origin of the Solar System
- Deformation and internal flow of a chondrule-precursor molten sphere in a shocked nebular gas
- Flow in a Liquid Sphere Moving with a Hypersonic Velocity in a Rarefied Gas : An Analytic Solution of Linearized Equations
- Shear instabilities in the dust layer of the solar nebula II. Different unperturbed states
- Shear instabilities in the dust layer of the solar nebula I. The linear analysis of a non-gravitating one-fluid model without the Coriolis and the solar tidal forces
- On the Peculiarity of the Pion in the Composite Model of Hadrons
- The Generalized Dual Loop Expansion of U(N_c) Gauge Theory
- Shear instabilities in the dust layer of the solar nebula III. Effects of the Coriolis force
- Condition for the formation of the compound chondrules in the solar nebula
- 206 A case of type II diabetes mellitus in a boy with panhypopituitalism
- 119 Influence of body weight increment from birth to 3 years of age for body weight indices, serum lipid, and leptin concentrations at 10 and 13 years old
- 136 Basal analysis of tissue-specific glucocorticoid metabolism : Approach from 11 β-hydroxysteroid dehydrogenase type 1 gene promoter analysis
- 134 The effects of diabetic pregnancy on fetal glucocorticoid and glucose metabolism in rats
- 179 DIFFERENT RESPONSIVENESS IN BODY WEIGHT TO 11β-HYDROXYSTEROID DEHYDROGENASE INHIBITION BY GLYCYRRHETINIC ACID IN OBESE AND LEAN ZUCKER RATS
- 177 SEXUAL DIFFERENCES IN THEIR CORRELATION BETWEEN SERUM LEPTIN CONCENTRATIONS AND INDICES OF BODY FAT AND WEIGHT : BODY MASS INDEX, PERCENTAGE OF OVERWEIGHT AND PERCENTAGE OF BODY FAT
- Thermal evolution of icy planetesimals in the solar nebula