Add to ORKGThe structure of the solar convection zone calculated according to the mixing length theory is found to be consistent with the transport of convective flux by a linear superposition of statistically independent unstable convective modes, provided the effects of turbulent conductivity and viscosity are taken into account. The resultant vertical velocity is in reasonable agreement with observed granular velocity in the atmosphere, but the horizontal velocity turns out to be too large for low l modes
A new mixing length scale is presented for turbulence closure schemes with special emphasis on neutr...
In this paper, we investigate the problem of supersonic convection caused by the application of the ...
Aims. We investigate the relation between 1D atmosphere models that rely on the mixing length theory...
The construction of solar or stellar models is hindered by the difficulty of computing, with suffici...
We compare the results of realistic numerical simulations of convection in the superadiabatic layer ...
We study the mixing length concept in comparison to three-dimensional numerical calculations of con...
Based on detailed 2D numerical radiation hydrodynamics calculations of time-dependent compressible c...
Radiation hydrodynamics (RHD) models provide detailed information about the dynamics, thermal struct...
. By simulating the convection in the upper layers of six different stars and matching these simulat...
We compute the rates P at which acoustic energy is injected into the solar radial p modes for sever...
Some alternatives to the traditional mixing-length theory (MLT) have recently been proposed for mode...
The stability of linear convective modes in the solar convection zone is investigated by incorporati...
The turbulent magnetic diffusivity in the solar convection zone is one of the most poorly constraine...
The effect of adjustments to the superadiabatic layer (SAL) in a model of the Sun on the p-mode osci...
We present a grid of numerical 2D radiation hydrodynamics (RHD) models of the solar-like surface con...
A new mixing length scale is presented for turbulence closure schemes with special emphasis on neutr...
In this paper, we investigate the problem of supersonic convection caused by the application of the ...
Aims. We investigate the relation between 1D atmosphere models that rely on the mixing length theory...
The construction of solar or stellar models is hindered by the difficulty of computing, with suffici...
We compare the results of realistic numerical simulations of convection in the superadiabatic layer ...
We study the mixing length concept in comparison to three-dimensional numerical calculations of con...
Based on detailed 2D numerical radiation hydrodynamics calculations of time-dependent compressible c...
Radiation hydrodynamics (RHD) models provide detailed information about the dynamics, thermal struct...
. By simulating the convection in the upper layers of six different stars and matching these simulat...
We compute the rates P at which acoustic energy is injected into the solar radial p modes for sever...
Some alternatives to the traditional mixing-length theory (MLT) have recently been proposed for mode...
The stability of linear convective modes in the solar convection zone is investigated by incorporati...
The turbulent magnetic diffusivity in the solar convection zone is one of the most poorly constraine...
The effect of adjustments to the superadiabatic layer (SAL) in a model of the Sun on the p-mode osci...
We present a grid of numerical 2D radiation hydrodynamics (RHD) models of the solar-like surface con...
A new mixing length scale is presented for turbulence closure schemes with special emphasis on neutr...
In this paper, we investigate the problem of supersonic convection caused by the application of the ...
Aims. We investigate the relation between 1D atmosphere models that rely on the mixing length theory...