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Precise Masses Reveal that TOI-700 c is Low Density and TOI-700 d is Rocky
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Possible Global Magneto-Fluid Structure of the Stellar Convection Zone
Possible Global Magneto-Fluid Structure of the Stellar Convection Zoneopenaire
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Nonlinear hydrodynamical models of stellar convective zones
Astrophysics and Space Science, 1986Large-eddy simulation (LES) of turbulent convection is discussed in various versions (mixing-length theory, modal theory and spectral theory) in respect to the application to stellar convective zones. For the model construction, the non-local mixing-length formalism is suitable. However, for the determination of basic flow patterns and of mixing-length,
Wasaburo Unno, Masa-Aki Kondo
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A note on anisotropic convection and the rotation of stellar convective zones
Astrophysics and Space Science, 1974The interaction of rotation and convection produces a latitude dependent anisotropic turbulent viscosity. When this friction is dominant, equilibrium of a convective outer layer of a star is achieved by an equatorial acceleration and a two-zone circulation, towards the equator at low surface latitudes.
I. Roxburgh
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Convective penetration into stellar radiation zones
2008We recall the evidence for convective penetration exhibited by geophysical fluids, laboratory experiments and computer simulations. A simple model is deduced from these observations, which serves to establish a relation between the subadiabatic extent of a convective region and the velocity of the penetrating motions.
J. Zahn
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On the Theoretical Treatment of Stellar Convection Zones
Publications of the Astronomical Society of Australia, 1970 The theory of stellar convection zones has met three difficult problems. They are non-linearity, non-locality, and non-greyness of radiative transport. Non-linearity is inherent in turbulence. Non-locality is due to the nature of convection, that larger eddies are apt to be more unstable as indicated by the fourth-power dependence of the Rayleigh ...
W. Unno
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Solar and stellar convection zones
Computer Physics Reports, 1990Abstract There are several important astrophysical questions that might be answered by numerical modelling. These involve the kinematic effects of motion on magnetic fields, the dynamics of magnetoconvection, the stucture and scale of convection and the global dynamo problem.
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Stellar Models with Isothermal Cores and Intermediate Convective Zones. II.
Publications of the Astronomical Society of Japan, 1957Abstract Stellar models consisting of isothermal cores exhausted of hydrogen and convective zones with intermediate hydrogen content surrounded by hydrogen-rich radiative envelopes are constructed. Six sequences of models with specified values of log C are computed for a fixed ratio of molecular weight of the core to that of the envelope.
Zyuiti Hitotuyanagi, Kazuo Suda
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Some properties of the kinetic energy flux and dissipation in turbulent stellar convection zones
, 2010We investigate simulated turbulent flow within thermally driven stellar convection zones. Different driving sources are studied, including cooling at the top of the convectively unstable region, as occurs in surface convection zones; and heating at the ...
C. Meakin, W. Arnett
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Pulsations Of Stellar Envelopes With Convection Zones.
1967PhD ; Astronomy ; Astrophysics ; University of Michigan, Horace H. Rackham School of Graduate Studies ; http://deepblue.lib.umich.edu/bitstream/2027.42/185041/2/6807576 ...
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