Results 31 to 40 of about 345 (250)
How plasma coupling and convective-zone depth shape the rotation of solar-mass stars
Astronomy & AstrophysicsContext. Stellar rotation on the main sequence is a complex function of mass and age, displaying multiple regimes whose physical origin remains only partially understood.
Brito A., Lopes I.
doaj +1 more source
Dynamos in Stellar Convection Zones: of Wreaths and Cycles [PDF]
Journal of Physics: Conference Series, 2011 10 pages, 5 figures, a4 format; proceedings for SOHO 24/GONG 2010 conference: "A new era of seismology of the Sun and solar-like stars," Aix-en-Provence, France, June 27-July 4, 2010 (JPCS)
openaire +2 more sources
The Astrophysical JournalTurbulent mixing remains one of the primary uncertainties in the modeling of stellar interiors. In stellar evolution simulations, regions where mixing occurs are typically identified using instability criteria. A particularly interesting situation arises
M. Miguel Ocampo +1 more
doaj +1 more source
Advanced Engineering Materials, EarlyView.A simplified thermoplastic pultrusion model is developed to predict thermal fields in glass fiber/polyethylene terephthalate (GF/PET) composites with reduced computational cost. By combining effective material homogenization, validation against literature data, and Gaussian‐process‐based optimization, the study reveals how heating limits, pulling speed,
Elder Soares +3 more
wiley +1 more source
Modelling Time-dependent Convective Penetration in 1D Stellar Evolution
The Astrophysical JournalOne-dimensional stellar evolution calculations produce uncertain predictions for quantities like the age, core mass, core compactness, and nucleosynthetic yields; a key source of uncertainty is the modeling of interfaces between regions that are ...
Cole Johnston +9 more
doaj +1 more source
Advanced Engineering Materials, EarlyView.A novel workflow for investigating hydride vapor phase epitaxy for GaN bulk crystal growth is proposed. It combines Design of experiments (DoE) with physical simulations of mass transport and crystal growth kinetics, serving as an intermediate step between DoE and experiments.
J. Tomkovič +7 more
wiley +1 more source
Differential Rotation in Stellar Convection Zones
The Astrophysical Journal, 1970 The analysis of an earlier paper (Busse l970a) in which the differential rotation of the Sun was explained as the result of large scale convection in the solar convection zone is extended to include the detailed spatial dependence of the meridional circulation as well as of the differential rotation.
openaire +1 more source
Numerical simulations of stellar convective dynamos III. At the base of the convection zone [PDF]
Geophysical & Astrophysical Fluid Dynamics, 1985 We describe numerical simulations of giant-cell solar convection and magnetic field generation. Nonlinear, three-dimensional, time-dependent solutions of the anelastic magnetohydrodynamic equations are presented for a stratified, rotating, spherical shell of ionized gas.
openaire +2 more sources
Advanced Engineering Materials, EarlyView.A combined experimental–computational framework identifies energy‐dependent laser absorptivity for NiTi in laser powder‐bed fusion, applicable to conduction and transition modes. Single‐track experiments and thermofluid smoothed particle hydrodynamics simulations are coupled through inverse analysis of melt pool geometry.
Mohamadreza Afrasiabi +3 more
wiley +1 more source
Twists in the flow: Revisiting convective mixing in rotating stellar models
Astronomy & AstrophysicsContext. Convection and rotation are both key processes in stellar evolution modelling. While standard mixing-length theory (MLT) provides a widely used modelling of convection, it neglects the effects of rotation on convective transport. Aims.
Agrawal Poojan +4 more
doaj +1 more source