Large-scale flow and transport of magnetic flux in the solar convection zone

2000 ◽  
Vol 21 (3-4) ◽  
pp. 315-318
Author(s):  
P. Ambrož
Keyword(s):  
Magnetic Flux ◽  
Large Scale ◽  
Convection Zone ◽  
Solar Convection Zone ◽  
Flow And Transport ◽  
Solar Convection ◽  
Large Scale Flow

Large-scale Flow and Transport of Magnetic Flux in the Solar Convection Zone

2000 ◽  
Vol 179 ◽  
pp. 315-318
Author(s):  
P. Ambrož
Keyword(s):  
Velocity Field ◽  
Magnetic Flux ◽  
Large Scale ◽  
Activity Cycle ◽  
Horizontal Displacement ◽  
Horizontal Velocity ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Activity Cycles ◽  
Large Scale Flow

AbstractHorizontal large-scale velocity field describes horizontal displacement of the photospheric magnetic flux in zonal and meridian directions. The flow systems of solar plasma, constructed according to the velocity field, create the large-scale cellular-like patterns with up-flow in the center and the down-flow on the boundaries. Distribution of the largescale horizontal eddies (with characteristic scale length from 350 to 490 Mm) was found in the broad equatorial zone, limited by 60° latitude circles on both hemispheres. The zonal averages of the zonal and meridian velocities, and the total horizontal velocity for each Carrington rotation during the activity cycles no. 21 and 22 varies during the 11-yr activity cycle. Plot of RMS values of total horizontal velocity is shifted about 1.6 years before the similarly shaped variation of the magnetic flux.

Large Scale Flows in the Solar Convection Zone

2008 ◽  
Vol 144 (1-4) ◽  
pp. 151-173 ◽  
Author(s):  
Allan Sacha Brun ◽  
Matthias Rempel
Keyword(s):  
Large Scale ◽  
Convection Zone ◽  
Solar Convection Zone ◽  
Solar Convection

scholarly journals The Rise of Kink-Unstable Magnetic Flux Tubes in the Solar Convection Zone

1998 ◽  
Vol 505 (1) ◽  
pp. L59-L63 ◽  
Author(s):  
Y. Fan ◽  
E. G. Zweibel ◽  
M. G. Linton ◽  
G. H. Fisher
Keyword(s):  
Magnetic Flux ◽  
Convection Zone ◽  
Solar Convection Zone ◽  
Flux Tubes ◽  
Solar Convection ◽  
Magnetic Flux Tubes

scholarly journals On the Detection of Subphotospheric Convective Velocities and Temperature Fluctuations

1983 ◽  
Vol 66 ◽  
pp. 401-410
Author(s):  
D. O. Gough ◽  
J. Toomre
Keyword(s):  
Large Scale ◽  
Temperature Fluctuations ◽  
Wave Number ◽  
Convective Velocity ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Wave Patterns ◽  
Large Scale Flow ◽  
Low Amplitude ◽  
High Degree

AbstractA procedure is outlined for estimating the influence of large-scale convective eddies on the wave patterns of five-minute oscillations of high degree. The method is applied to adiabatic oscillations, with frequency ω and wave number k, of a plane-parallel polytropic layer upon which is imposed a low-amplitude convective flow. The distortion to the k – ω relation has two constituents: one depends on the horizontal component of the convective velocity and has a sign which depends on the sign of ω/k; the other depends on temperature fluctuations and is independent of the sign of ω/k. The magnitude of the distortion is just at the limit of present observational sensitivity. Thus there is reasonable hope that it will be possible to reveal some aspects of the large-scale flow in the solar convection zone

scholarly journals Helicity–vorticity turbulent pumping of magnetic fields in the solar dynamo

2012 ◽  
Vol 8 (S294) ◽  
pp. 367-368
Author(s):  
V. V. Pipin
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Differential Rotation ◽  
Large Scale ◽  
Convection Zone ◽  
Solar Dynamo ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Large Scale Magnetic Field ◽  
Convective Motions

AbstractThe interaction of helical convective motions and differential rotation in the solar convection zone results in turbulent drift of a large-scale magnetic field. We discuss the pumping mechanism and its impact on the solar dynamo.

scholarly journals Loss of toroidal magnetic flux by emergence of bipolar magnetic regions

2020 ◽  
Vol 636 ◽  
pp. A7
Author(s):  
R. H. Cameron ◽  
M. Schüssler
Keyword(s):  
Solar Cycle ◽  
Magnetic Flux ◽  
Decay Time ◽  
Loss Rate ◽  
Convection Zone ◽  
Flux Emergence ◽  
Simple Estimate ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Flux Loss

The polarity of the toroidal magnetic field in the solar convection zone periodically reverses in the course of the 11/22-year solar cycle. Among the various processes that contribute to the removal of “old-polarity” toroidal magnetic flux is the emergence of flux loops forming bipolar regions at the solar surface. We quantify the loss of subsurface net toroidal flux by this process. To this end, we determine the contribution of an individual emerging bipolar loop and show that it is unaffected by surface flux transport after emergence. Together with the linearity of the diffusion process this means that the total flux loss can be obtained by adding the contributions of all emerging bipolar magnetic regions. The resulting total loss rate of net toroidal flux amounts to 1.3 × 1015 Mx s−1 during activity maxima and 6.1 × 1014 Mx s−1 during activity minima, to which ephemeral regions contribute about 90 and 97%, respectively. This rate is consistent with the observationally inferred loss rate of toroidal flux into interplanetary space and corresponds to a decay time of the subsurface toroidal flux of about 12 years, also consistent with a simple estimate based on turbulent diffusivity. Consequently, toroidal flux loss by flux emergence is a relevant contribution to the budget of net toroidal flux in the solar convection zone. The consistency between the toroidal flux loss rate due to flux emergence and what is expected from turbulent diffusion, and the similarity between the corresponding decay time and the length of the solar cycle are important constraints for understanding the solar cycle and the Sun’s internal dynamics.

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