| タイトル | The role of turbulent convection in the primitive solar nebula. I - Theory. II - Results |
| 著者（英） | Hubickyj, O.; Cabot, W.; Canuto, V. M.; Pollack, J. B. |
| 著者所属（英） | NASA Goddard Inst. for Space Studies|NASA Ames Research Center |
| 発行日 | 1987-03-01 |
| 言語 | eng |
| 内容記述 | A model of convective turbulence which takes radiative dissipation, rotation, and convective motion anisotropy into account, on the basis of a closure for the nonlinear interactions that employs the growth rates of hydrodynamic instabilities, is used to obtain a theoretical framework for modeling the primordial solar nebula. It is assumed that convection is the sole source of turbulence causing the solar nebula to evolve. Vertical structure equations in the thin disk approximation are developed and a detailed comparison with the previous solar nebula convective models of such workers as Lin et al. (1981, 1982) is undertaken. The present values for the turbulent efficiency are much lower and more sensitive to opacity and surface density, resulting in low turbulent speeds, a more massive disk, a lower accretion rate 'best value', and a longer characteristic dispersal time for the disk. It is concluded that convection may not be the dominant source of turbulence needed to evolve young solar/stellar nebulae. |
| NASA分類 | ASTROPHYSICS |
| レポートNO | 87A37260 |
| 権利 | Copyright |
| URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/378155 |
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