Miroslav Mocák
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View article: Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase
Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase Open
Our understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models c…
View article: Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations
Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations Open
One-dimensional (1D) stellar evolution models are widely used across various astrophysical fields, however they are still dominated by important uncertainties that deeply affect their predictive power. Among those, the merging of independe…
View article: Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations
Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations Open
One-dimensional (1D) stellar evolution models are widely used across various astrophysical fields, however they are still dominated by important uncertainties that deeply affect their predictive power. Among those, the merging of independe…
View article: 3D simulations of a neon burning convective shell in a massive star
3D simulations of a neon burning convective shell in a massive star Open
The treatment of convection remains a major weakness in the modelling of stellar evolution with one-dimensional (1D) codes. The ever-increasing computing power makes now possible to simulate in three-dimensional (3D) part of a star for a f…
View article: 3D simulations of convective shell Neon-burning in a massive star
3D simulations of convective shell Neon-burning in a massive star Open
The treatment of convection remains a major weakness in the modelling of stellar evolution with one-dimensional (1D) codes. The ever increasing computing power makes now possible to simulate in 3D part of a star for a fraction of its life,…
View article: 3D hydrodynamics simulations of massive stars with the PROMPI code
3D hydrodynamics simulations of massive stars with the PROMPI code Open
Evolutionary models of massive stars are affected by uncertainties related to three-dimensional processes like convection. However, it is not computationally possible to simulate at the same time both the entire lifetime of a star and its …
View article: Dynamics in a stellar convective layer and at its boundary: Comparison of five 3D hydrodynamics codes
Dynamics in a stellar convective layer and at its boundary: Comparison of five 3D hydrodynamics codes Open
Our ability to predict the structure and evolution of stars is in part limited by complex, 3D hydrodynamic processes such as convective boundary mixing. Hydrodynamic simulations help us understand the dynamics of stellar convection and con…
View article: 3D Simulations and MLT: II. Onsager's Ideal Turbulence
3D Simulations and MLT: II. Onsager's Ideal Turbulence Open
We simulate stellar convection at high Reynolds number (Re$\lesssim$7000) with causal time stepping but no explicit viscosity. We use the 3D Euler equations with shock capturing (Colella & Woodward 1984). Anomalous dissipation of turbulent…
View article: 3D simulations and MLT: II. RA-ILES results
3D simulations and MLT: II. RA-ILES results Open
Extending (\citealt{alvio1}), we analyze the physics of the turbulent cascade in stars. Our simulations give an asymptotic limit for the global damping length for turbulent kinetic energy, $\ld \sim \langle u^3 \rangle /\langle \epsilon \r…
View article: Turbulent mixing and nuclear burning in stellar interiors
Turbulent mixing and nuclear burning in stellar interiors Open
The turbulent burning of nuclei is a common phenomenon in the evolution of\nstars. Here we examine a challenging case: the merging of the neon and oxygen\nburning shells in a 23 M$_{\\odot}$ star. A previously unknown quasi-steady\nstate i…