Chapter 11 Cooling of the Solar Nebula : Part IV Physical Processes in the Solar Nebula : Origin of the Solar System
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概要
- 論文の詳細を見る
In the study of planetary formation one of the most important problem is that the solar nebula was turbulent or not: In turbulent nebula effective viscosity induces the radial mass infall, whereas there is no radial mass transport in the quiescent nebula. To sustain turbulence of any kind one needs some triggering instabilities. Thermal convection is thought to be the most well-examined candidate for the instabilities. Then the question is:how long did the convection continue in the solar nebula? In this chapter we will review our recent study on the quasi-static vertical contraction of the nebula due to radiative cooling in order to clarify the evolution of the vertical structure, especially duration of convection. We first estimate the maximum temperature due to shock heating of infalling matter (about 1400K in Earth's region). Next we perform one-dimensional numerical simulation of quasi-static contraction of the cooling nebula under the assumption that the solar radiation is incident on the surface of the nebula. We find this surface heating stabilizes the convection of the nebula at least near Earth's region. On the contrary in the outer region solar radiation is very weak, so that convection would continue longer than that in Earth's region. We discuss a solar nebula where quiescent regions and turbulent ones coexist along the radial direction.
- 理論物理学刊行会の論文
- 1989-03-10
著者
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Nakagawa Y
Department Of Earth And Planetary Sciences Faculty Of Science Kobe University
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Nakagawa Yoshitsugu
Geophysical Institute University Of Tokyo
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Nakagawa Yoshitsugu
Geophysical Institute Faculty Of Science University Of Tokyo
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WATANABE Sei-ichiro
Geophysical Institute, University of Tokyo
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Watanabe Sei-ichiro
Geophysical Institute University Of Tokyo
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NAKAGAWA Yoshitsugu
Department of Physics, Kyoto University
関連論文
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- 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
- 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
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