Simulations of Core Convection in Rotating A-Type Stars: Differential Rotation and Overshooting

@article{Browning2003SimulationsOC,
  title={Simulations of Core Convection in Rotating A-Type Stars: Differential Rotation and Overshooting},
  author={Matthew Keith Morris Browning and Allan Sacha Brun and J. Toomre},
  journal={The Astrophysical Journal},
  year={2003},
  volume={601},
  pages={512-529}
}
We present the results of three-dimensional simulations of core convection within A-type stars of 2 M☉, at a range of rotation rates. We consider the inner 30% by radius of such stars, thereby encompassing the convective core and some of the surrounding radiative envelope. We utilize our anelastic spherical harmonic code, which solves the compressible Navier-Stokes equations in the anelastic approximation, to examine highly nonlinear flows that can span multiple scale heights. The cores of… 
Simulations of Core Convection in Rotating A-Type Stars: Magnetic Dynamo Action
Core convection and dynamo activity deep within rotating A-type stars of 2 M☉ are studied with three-dimensional nonlinear simulations. Our modeling considers the inner 30% by radius of such stars,
Simulations of Dynamo Action in Fully Convective Stars
We present three-dimensional nonlinear magnetohydrodynamic simulations of the interiors of fully convective M dwarfs. Our models consider 0.3 solar-mass stars using the Anelastic Spherical Harmonic
Simulations of turbulent convection in rotating young solarlike stars : Differential rotation and meridional circulation
We present the results of three-dimensional simulations of the deep convective envelope of a young (10 Myr) 1 M? star, obtained with the anelastic spherical harmonic code. Since young stars are known
On the Dynamics of Overshooting Convection in Spherical Shells: Effect of Density Stratification and Rotation
Overshooting of turbulent motions from convective regions into adjacent stably stratified zones plays a significant role in stellar interior dynamics, as this process may lead to mixing of chemical
NUMERICAL SIMULATIONS OF A ROTATING RED GIANT STAR. I. THREE-DIMENSIONAL MODELS OF TURBULENT CONVECTION AND ASSOCIATED MEAN FLOWS
With the development of one-dimensional stellar evolution codes including rotation and the increasing number of observational data for stars of various evolutionary stages, it becomes more and more
MODELING THE DYNAMICAL COUPLING OF SOLAR CONVECTION WITH THE RADIATIVE INTERIOR
The global dynamics of a rotating star like the Sun involves the coupling of a highly turbulent convective envelope overlying a seemingly benign radiative interior. We use the anelastic spherical
A Model of Rotating Convection in Stellar and Planetary Interiors. I. Convective Penetration
A monomodal model for stellar and planetary convection is derived for the magnitude of the rms velocity, degree of superadiabaticity, and characteristic length scale as a function of rotation rate as
Simulation of turbulent convection in a slowly rotating red giant star
The first 3-D non-linear hydrodynamical simulation of the inner convective envelope of a rotating low mass red giant star is presented. This simulation, computed with the ASH code, aims at
Exploring the deep convection and magnetism of A-type stars
Abstract A-type stars have both a near-surface layer of fast convection that can excite acoustic modes and a deep zone of core convection whose properties may be probed with asteroseismology. Many
Assessing the Deep Interior Dynamics and Magnetism of A-type Stars
A-type stars have both a shallow near-surface zone of fast convection that can excite acoustic modes and a deep zone of core convection whose properties may be studied through asteroseismology. Many
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 60 REFERENCES
Turbulent Convection under the Influence of Rotation: Sustaining a Strong Differential Rotation
The intense turbulence present in the solar convection zone is a major challenge to both theory and simulation as one tries to understand the origins of the striking differential rotation profile
Stellar convection theory. III - Dynamical coupling of the two convection zones in A-type stars by penetrative motions
Anelastic modal equations are used to examine thermal convection occurring over many density scale heights in the entire outer envelope of an A-type star, encompassing both the hydrogen and helium
Turbulent Compressible Convection with Rotation. II. Mean Flows and Differential Rotation
The e†ects of rotation on turbulent, compressible convection within stellar envelopes are studied through three-dimensional numerical simulations conducted within a local f-plane model. This work
Turbulent Solar Convection and its Coupling with Rotation
The dynamics of the vigorous convection in the outer envelope of the Sun must determine the transport of energy, angular momentum, and magnetic fields and must therefore be responsible for the
Model calculations concerning rotation at high solar latitudes and the depth of the solar convection zone
The author has previously carried out extensive nonlinear numerical simulations of convection in a rotating spherical shell, motivated by the problem of understanding the Sun's differential rotation.
Three-dimensional Spherical Simulations of Solar Convection. I. Differential Rotation and Pattern Evolution Achieved with Laminar and Turbulent States
Rotationally constrained convection possesses velocity correlations that transport momentum and drive mean —ows such as diUerential rotation. The nature of this transport can be very complex in
Nonlinear dynamics of boussinesq convection in a deep rotating spherical shell II: Effects of temperature boundary conditions
Abstract We examine the influence on convection in a rotating spherical shell of various boundary conditions on temperature. In particular, we look at the response to constant heat flux, or fixed
Penetration and Overshooting in Turbulent Compressible Convection
We present the results of a series of high-resolution, three-dimensional numerical experiments that investigate the nature of turbulent compressible convective motions extending from a convection
Penetration below a convective zone
Two-dimensional numerical simulations are used to investigate how fully compressible nonlinear convection penetrates into a stably stratified zone beneath a stellar convection zone. Estimates are
The Internal Rotation of the Sun
▪ 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 been built up of the
...
1
2
3
4
5
...