▪ Abstract In this article we first review the main physical effects to be considered in the
building of evolutionary models of rotating stars on the Upper Main-Sequence (MS). The …

▪ Abstract Helioseismology has transformed our knowledge of the Sun's rotation. Earlier
studies revealed the Sun's surface rotation, but now a detailed observational picture has …

The past few decades have seen dramatic progress in our understanding of solar interior
dynamics, prompted by the relatively new science of helioseismology and increasingly …

We present a self-consistent model for stellar turbulent convection that is similar in spirit to
the CM model (Canuto & Mazzitelli 1991) since it accounts for the full spectrum of the …

Observers have long measured solar rotation with different techniques and obtained
different results. This paper compares differential rotation measurements from four …

Magnetism is one of the most pervasive features of the Universe, with planets, stars and
entire galaxies all having associated magnetic fields. All of these fields are generated by the …

The global scales of solar convection are studied through three-dimensional simulations of
compressible convection carried out in spherical shells of rotating fluid that extend from the …

Stars can be fascinating settings in which to study intricate couplings among convection,
rotation, magnetism, and shear, usually under distinctly nonlinear conditions that yield …

The ages of the oldest stars in our Galaxy can be estimated by comparing stellar populations
in globular clusters to calibrated stellar models. The best data give cluster ages of about …

In this paper, we introduce the concept of direct statistical simulation for astrophysical flows.
This technique may be appropriate for problems in astrophysical fluids where the …