Solar and stellar convection zones

1990 ◽  
Vol 12 (4) ◽  
pp. 233-245 ◽  
Author(s):  
N.O. Weiss
Keyword(s):  
Stellar Convection

scholarly journals Possible Global Magneto-Fluid Structure of the Stellar Convection Zone

2006 ◽  
Vol 58 (3) ◽  
pp. 605-616 ◽  
Author(s):  
Sanae I. Itoh ◽  
Kimitaka Itoh ◽  
Patrick H. Diamond ◽  
Akira Yoshizawa
Keyword(s):  
Convection Zone ◽  
Fluid Structure ◽  
Stellar Convection

Connecting a Star’s Convection Zone with its Corona

1995 ◽  
Vol 12 (2) ◽  
pp. 180-185 ◽  
Author(s):  
D. J. Galloway ◽  
C. A. Jones
Keyword(s):  
Magnetic Field ◽  
Convection Zone ◽  
Flux Rope ◽  
Field System ◽  
Stellar Convection ◽  
Coronal Activity ◽  
Flux Concentration ◽  
Global Understanding ◽  
The Magnetic Field

AbstractThis paper discusses problems which have as their uniting theme the need to understand the coupling between a stellar convection zone and a magnetically dominated corona above it. Interest is concentrated on how the convection drives the atmosphere above, loading it with the currents that give rise to flares and other forms of coronal activity. The role of boundary conditions appears to be crucial, suggesting that a global understanding of the magnetic field system is necessary to explain what is observed in the corona. Calculations are presented which suggest that currents flowing up a flux rope return not in the immediate vicinity of the rope but rather in an alternative flux concentration located some distance away.

Laboratory Experiments on Planetary and Stellar Convection Performed on Spacelab 3

Science ◽  
1986 ◽  
Vol 234 (4772) ◽  
pp. 61-64 ◽  
Author(s):  
J. E. HART ◽  
J. TOOMRE ◽  
A. E. DEANE ◽  
N. E. HURLBURT ◽  
G. A. GLATZMAIER ◽  
...  
Keyword(s):  
Laboratory Experiments ◽  
Stellar Convection

scholarly journals Stellar Convection as a Low Prandtl Number Flow

1991 ◽  
Vol 130 ◽  
pp. 57-61
Author(s):  
Josep M. Massaguer
Keyword(s):  
Nusselt Number ◽  
Prandtl Number ◽  
Heat Transport ◽  
Large Scale ◽  
Shear Layers ◽  
Turbulent Convection ◽  
The Sun ◽  
Stellar Convection ◽  
Cool Stars ◽  
Number Flow

AbstractThermal convection in the Sun and cool stars is often modeled with the assumption of an effective Prandtl number σ ≃ 1. Such a parameterization results in masking of the presence of internal shear layers which, for small σ, might control the large scale dynamics. In this paper we discuss the relevance of such layers in turbulent convection. Implications for heat transport – i.e. for the Nusselt number power law – are also discussed.

scholarly journals 3-D Convection Models: Are They Compatible with 1-D Models?

2000 ◽  
Vol 176 ◽  
pp. 362-372
Author(s):  
Å. Nordlund ◽  
R. F. Stein
Keyword(s):  
Numerical Modeling ◽  
Energy Transport ◽  
Three Dimensional ◽  
Stellar Structure ◽  
Surface Layers ◽  
Stellar Convection ◽  
Fair Representation ◽  
Dimensional Models ◽  
Three Dimensional Models ◽  
Hr Diagram

AbstractWe review properties of stellar convection, as derived from detailed 3-D numerical modeling, and assess to what extent 1-D models are able to provide a fair representation of stellar structure in various regions of the HR diagram. We point out a number of problems and discrepancies that are inevitable when using conventional 1-D models. The problems originate mainly in the surface layers, where horizontal fluctuations become particularly large, and where convective energy transport gives way to radiation. We conclude that it is necessary (and possible) to use three-dimensional models of these layers, in order to avoid the uncertainties and inaccuracies associated with 1-D representations.

scholarly journals Linking Thin Flux Tube MHD Models to Apparent Stellar Surface Activity

2004 ◽  
Vol 219 ◽  
pp. 546-551
Author(s):  
T. Granzer ◽  
K. G. Strassmeier
Keyword(s):  
Magnetic Flux ◽  
Surface Activity ◽  
Flux Tube ◽  
Convection Zone ◽  
Active Regions ◽  
Similar Model ◽  
Flux Tubes ◽  
Stellar Convection ◽  
Magnetic Flux Tubes ◽  
Spot Formation

We model thin magnetic flux tubes as they rise from the bottom of a stellar convection zone to the photosphere. On emergence they form active regions, i.e. star spots. This model was very successfully applied to the solar case, where the simulations where in agreement with the butterfly diagram, Joy's law, and Hale's law. We propose the use of a similar model to describe stellar activity in the more extreme form found on active stars. A comparison between Doppler-images of well-observed pre-MS stars and a theoretically derived probability of star-spot formation as a function of latitude is presented.

scholarly journals Test of a New Theory for Stellar Convection using Helioseismology

1993 ◽  
Vol 137 ◽  
pp. 63-65
Author(s):  
L. Paternó ◽  
R. Ventura ◽  
V.M. Canuto ◽  
I. Mazzitelli
Keyword(s):  
Reaction Rates ◽  
Turbulent Convection ◽  
Standard Theory ◽  
Evolutionary Models ◽  
Mixing Length ◽  
Surface Layers ◽  
Stellar Convection ◽  
The Standard Model ◽  
Convection Model ◽  
Mixing Length Theory

AbstractTwo evolutionary models of the Sun have been tested using helioseismological data. The two models use the same input micro-physics (nuclear reaction rates, opacity, equation of state) and the same numerical evolutionary code, but differ in the treatment of turbulent convection. The first model employs the standard mixing - length theory of convection, while the second one employs a new turbulent convection model which overcomes some basic inconsistencies of the standard theory of convection.The test rests on the calculation of p-mode eigenfrequencies and on the comparison with the helioseismological data.The comparison shows an overall improvement of the eigenfrequencies calculated with the new model with respect to those calculated with the standard model, although it appears that both models still suffer from inaccuracies especially in the treatment of the surface layers.

Sign in / Sign up

Export Citation Format

Share Document