The Dynamo Mechanism in the Deep Convection Zone of the Sun

1994 ◽  
pp. 249-256 ◽  
Author(s):  
T. Prautzsch
Keyword(s):  
Convection Zone ◽  
Deep Convection ◽  
The Sun ◽  
Dynamo Mechanism

scholarly journals Can we detect convection in the Sun?

2006 ◽  
Vol 2 (S239) ◽  
pp. 364-369
Author(s):  
Shravan M. Hanasoge ◽  
T. L. Duvall ◽  
M. L. Derosa ◽  
M. S. Miesch
Keyword(s):  
Velocity Profile ◽  
Travel Time ◽  
Convection Zone ◽  
Deep Convection ◽  
Wave Flow ◽  
The Sun ◽  
Convective Flows ◽  
Flow Interaction ◽  
Propagating Waves

AbstractWe investigate the possibility of detecting deep convection in the Sun by computing travel-time shifts induced by convective flows interacting with propagating waves. The convection zone is modeled using a velocity profile taken from an Anelastic convection simulation. We present results obtained from a ray calculation of travel-time shifts. We compare these results with a full 3D calculation of the wave-flow interaction.

scholarly journals Soil Moisture Impacts on Convective Margins

2009 ◽  
Vol 10 (4) ◽  
pp. 1026-1039 ◽  
Author(s):  
Benjamin R. Lintner ◽  
J. David Neelin
Keyword(s):  
Soil Moisture ◽  
Hot Spots ◽  
Land Surface ◽  
Convection Zone ◽  
Deep Convection ◽  
Radiative Heating ◽  
Convective Parameterization ◽  
Surface Atmosphere ◽  
Moisture Conditions ◽  
Land Region

Abstract An idealized prototype for the location of the margins of tropical land region convection zones is extended to incorporate the effects of soil moisture and associated evaporation. The effect of evaporation, integrated over the inflow trajectory into the convection zone, is realized nonlocally where the atmosphere becomes favorable to deep convection. This integrated effect produces “hot spots” of land surface–atmosphere coupling downstream of soil moisture conditions. Overall, soil moisture increases the variability of the convective margin, although how it does so is nontrivial. In particular, there is an asymmetry in displacements of the convective margin between anomalous inflow and outflow conditions that is absent when soil moisture is not included. Furthermore, the simple cases presented here illustrate how margin sensitivity depends strongly on the interplay of factors, including net top-of-the-atmosphere radiative heating, the statistics of inflow wind, and the convective parameterization.

scholarly journals Magnetoconvection Patterns in Rotating Convection Zones

1991 ◽  
Vol 130 ◽  
pp. 37-56
Author(s):  
Paul H. Roberts
Keyword(s):  
Convection Zone ◽  
Solar Surface ◽  
Giant Cells ◽  
Conclusive Evidence ◽  
The Other ◽  
The Sun ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Entire Thickness ◽  
Convective Motions

AbstractIn addition to the well-known granulation and supergranulation of the solar convection zone (the “SCZ”), the presence of so-called “giant cells” has been postulated. These are supposed span the entire thickness of the SCZ and to stretch from pole to pole in a sequence of elongated cells like a “cartridge belt” or a bunch of “bananas” strung uniformly round the Sun. Conclusive evidence for the existence of such giant cells is still lacking, despite strenuous observational efforts to find them. After analyses of sunspot motion, Ribes and others believe that convective motions near the solar surface occurs in a pattern that is the antithesis of the cartridge belt: a system of “toroidal” or “doughnut” cells, girdling the Sun in a sequence that extends from one pole to the other. Galloway, Jones and Roberts have recently tried to meet the resulting theoretical challenge, with the mixed success reported in this paper.

scholarly journals Sunspot seismology

1988 ◽  
Vol 123 ◽  
pp. 181-182
Author(s):  
John H. Thomas ◽  
Bruce W. Lites ◽  
Toufik E. Abdelatif
Keyword(s):  
Theoretical Analysis ◽  
Observational Study ◽  
Convection Zone ◽  
The Sun ◽  
Full Account ◽  
Sunspot Umbra

The 5 minute oscillations in a sunspot umbra are the response of the sunspot to forcing by the 5 minute p-modes in the surrounding convection zone (Thomas 1981). This interaction of solar p-modes with a sunspot can be used to probe the structure of a sunspot beneath the visible surface of the Sun (Thomas, Cram, and Nye 1982). Here we report briefly the results of both an observational study and a simple theoretical analysis of this interaction. A full account of these results will be published elsewhere (Abdelatif, Lites, and Thomas 1986; Abdelatif and Thomas 1987).

scholarly journals Weak influence of near-surface layer on solar deep convection zone revealed by comprehensive simulation from base to surface

2019 ◽  
Vol 5 (1) ◽  
pp. eaau2307 ◽  
Author(s):  
H. Hotta ◽  
H. Iijima ◽  
K. Kusano
Keyword(s):  
Convection Zone ◽  
Solar Surface ◽  
Deep Convection ◽  
Surface Region ◽  
Local Domain ◽  
Near Surface ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Weak Influence ◽  
The Magnetic Field

The solar convection zone is filled with turbulent convection in highly stratified plasma. Several theoretical and observational studies suggest that the numerical calculations overestimate the convection velocity. Since all deep convection zone calculations exclude the solar surface due to substantial temporal and spatial scale separations, the solar surface, which drives the thermal convection with efficient radiative cooling, has been thought to be the key to solve this discrepancy. Thanks to the recent development in massive supercomputers, we are successful in performing the comprehensive calculation covering the whole solar convection zone. We compare the results with and without the solar surface in the local domain and without the surface in the full sphere. The calculations do not include the rotation and the magnetic field. The surface region has an unexpectedly weak influence on the deep convection zone. We find that just including the solar surface cannot solve the problem.

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