For solving time-dependent convection-dominated partial differential equations (PDEs),
which arise frequently in computational physics, high order numerical methods, including …

The review considers the modelling process for stellar convection rather than specific
astrophysical results. For achieving reasonable depth and length we deal with …

Context. Traditional one-dimensional hydrostatic model atmospheres introduce systematic
modelling errors into spectroscopic analyses of FGK-type stars. Aims. We present an …

Context. In the interior of stars, a convectively unstable zone typically borders a zone that is
stable to convection. Convective motions can penetrate the boundary between these zones …

We present results of a large, high-resolution 3D hydrodynamical simulation of the surface
layers of a DA white dwarf (WD) with T eff= 11 800 K and log (g)= 8 using the antares code …

Context. A 1D description of stellar dynamics is at the basis of stellar evolution modeling.
Designed to investigate open problems in stellar evolution, the MUltidimensional Stellar …

We present the first grid of 3D simulations for the pure-helium atmospheres of DB white
dwarfs. The simulations were computed with the co5bold radiation-hydrodynamics code and …

In this paper, we present corrections to the spectroscopic parameters of DB and DBA white
dwarfs with− 10.0≤ log (H/He)≤− 2.0, 7.5≤ log g≤ 9.0, and≲ T eff, based on 282 3D …

Context. Studies of stellar convection typically use a spherical-shell geometry. The radial
extent of the shell and the boundary conditions applied are based on the model of the star …

We present evolutionary models for solar-like stars with an improved treatment of convection
that results in a more accurate estimate of the radius and effective temperature. This is …