Magnetism, dynamo action and the solar-stellar connection
AS Brun, MK Browning - Living Reviews in Solar Physics, 2017 - Springer
The Sun and other stars are magnetic: magnetism pervades their interiors and affects their
evolution in a variety of ways. In the Sun, both the fields themselves and their influence on …
evolution in a variety of ways. In the Sun, both the fields themselves and their influence on …
Convective boundary mixing in main-sequence stars: theory and empirical constraints
EH Anders, MG Pedersen - Galaxies, 2023 - mdpi.com
The convective envelopes of solar-type stars and the convective cores of intermediate-and
high-mass stars share boundaries with stable radiative zones. Through a host of processes …
high-mass stars share boundaries with stable radiative zones. Through a host of processes …
A study of convective core overshooting as a function of stellar mass based on two-dimensional hydrodynamical simulations
I Baraffe, J Clarke, A Morison… - Monthly Notices of …, 2023 - academic.oup.com
We perform two-dimensional (2D) numerical simulations of core convection for zero-age
main-sequence stars covering a mass range from 3 to 20 M⊙. The simulations are …
main-sequence stars covering a mass range from 3 to 20 M⊙. The simulations are …
Simulations of solar and stellar dynamos and their theoretical interpretation
We review the state of the art of three dimensional numerical simulations of solar and stellar
dynamos. We summarize fundamental constraints of numerical modelling and the …
dynamos. We summarize fundamental constraints of numerical modelling and the …
The shape of convective core overshooting from gravity-mode period spacings
Context. The evolution of stars born with a convective core is highly dependent on the
efficiency and extent of near core mixing processes, which effectively increases both the …
efficiency and extent of near core mixing processes, which effectively increases both the …
3D hydrodynamic simulations of massive main-sequence stars–I. Dynamics and mixing of convection and internal gravity waves
We performed 3D hydrodynamic simulations of the inner radial extent of a star in the early
phase of the main sequence and investigate core convection and internal gravity waves in …
phase of the main sequence and investigate core convection and internal gravity waves in …
Turbulent dynamo action and its effects on the mixing at the convective boundary of an idealized oxygen-burning shell
G Leidi, R Andrassy, J Higl, PVF Edelmann… - Astronomy & …, 2023 - aanda.org
Convection is one of the most important mixing processes in stellar interiors. Hydrodynamic
mass entrainment can bring fresh fuel from neighboring stable layers into a convection zone …
mass entrainment can bring fresh fuel from neighboring stable layers into a convection zone …
Turbulence with large thermal and compositional density variations
D Livescu - Annual Review of Fluid Mechanics, 2020 - annualreviews.org
Density variations in fluid flows can arise due to acoustic or thermal fluctuations,
compositional changes during mixing of fluids with different molar masses, or phase …
compositional changes during mixing of fluids with different molar masses, or phase …
An atlas of convection in main-sequence stars
Convection is ubiquitous in stars and occurs under many different conditions. Here we
explore convection in main-sequence stars through two lenses: dimensionless parameters …
explore convection in main-sequence stars through two lenses: dimensionless parameters …
Towards a self-consistent model of the convective core boundary in upper main sequence stars-I. 2.5 D and 3D simulations
R Andrassy, G Leidi, J Higl, PVF Edelmann… - Astronomy & …, 2024 - aanda.org
There is strong observational evidence that the convective cores of intermediate-mass and
massive main sequence stars are substantially larger than those predicted by standard …
massive main sequence stars are substantially larger than those predicted by standard …