Statistics – Computation
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...358..282w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 358, July 20, 1990, p. 282-292.
Statistics
Computation
14
Contraction, Cooling, Gravitational Collapse, Nebulae, Solar System, Solar Temperature, Star Formation, Boundary Value Problems, Computational Astrophysics, Convection, Entropy, Hydrostatics, Opacity, Turbulence
Scientific paper
The evolution of the primitive solar nebula in the quasi-static contraction phase where the nebula cools down toward the thermal steady state is studied. The solar irradiation onto the nebula keeps the surface temperature constant, so that the convective ozone retreats from the surface as the nebula cools. Thus if thermal convection is the only source of turbulence, convection will quiet down in an early time of the cooling. Afterward, the nebula evolves toward an isothermal structure in a time scale of 1000 yr. The cooling rates in the vicinity of the midplate at 1 AU are 0.003 K/hr at T(c) = 1000 K and 3 x 10 to the -5th K/hr at T(c) = 300 K for the standard model. If some turbulence exists irrespective of convection, convection may continue for sufficiently strong turbulent heating.
Nakagawa Yoshitsugu
Nakazawa Kiyoshi
Watanabe Sei-ichiro
No associations
LandOfFree
Cooling and quasi-static contraction of the primitive solar nebula after gas accretion does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Cooling and quasi-static contraction of the primitive solar nebula after gas accretion, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Cooling and quasi-static contraction of the primitive solar nebula after gas accretion will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1092975