Solar wind and coronal structure near sunspot minimum: Pioneer and SMM observations from 1985–1987

1990 ◽  
Vol 95 (A6) ◽  
pp. 8231 ◽  
Author(s):  
J. D. Mihalov ◽  
A. Barnes ◽  
A. J. Hundhausen ◽  
E. J. Smith
Keyword(s):  
Solar Wind ◽  
Coronal Structure ◽  
Sunspot Minimum

scholarly journals Small Solar Wind Transients and Their Connection to the Large-Scale Coronal Structure

Solar Physics ◽  
2009 ◽  
Vol 256 (1-2) ◽  
pp. 327-344 ◽  
Author(s):  
E. K. J. Kilpua ◽  
J. G. Luhmann ◽  
J. Gosling ◽  
Y. Li ◽  
H. Elliott ◽  
...  
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Coronal Structure

scholarly journals Coronal Structure and Solar Wind

1980 ◽  
Vol 91 ◽  
pp. 73-78
Author(s):  
J. N. Tandon
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Coronal Holes ◽  
Solar Magnetic Fields ◽  
Coronal Structure ◽  
Active Centers ◽  
Hydromagnetic Wave ◽  
Field Lines ◽  
Open Magnetic Field ◽  
Coronal Structures

Recent observations of large scale coronal structures and solar wind have been studied. The intercorrelation of the two have been qualitatively explained through the focussing of solar-ion streams taking account of the local and general solar magnetic fields. This explains the association of coronal holes with weak, diverging open magnetic field lines and envisages the transfer of hydromagnetic wave energy from nearby active centers to account for the enhanced outflow of solar wind associated with coronal holes.

scholarly journals FADING CORONAL STRUCTURE AND THE ONSET OF TURBULENCE IN THE YOUNG SOLAR WIND

2016 ◽  
Vol 828 (2) ◽  
pp. 66 ◽  
Author(s):  
C. E. DeForest ◽  
W. H. Matthaeus ◽  
N. M. Viall ◽  
S. R. Cranmer
Keyword(s):  
Solar Wind ◽  
Coronal Structure ◽  
Onset Of Turbulence

scholarly journals Heliospheric Magnetic Field Configuration and its Coronal Sources

2001 ◽  
Vol 203 ◽  
pp. 585-594 ◽  
Author(s):  
T. H. Zurbuchen
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Cycle ◽  
Differential Rotation ◽  
Field Configuration ◽  
The Sun ◽  
Coronal Structure ◽  
Magnetic Field Configuration ◽  
Archimedean Spiral ◽  
Heliospheric Magnetic Field

The heliospheric magnetic field configuration is largely determined in the solar atmosphere. The interplanetary magnetic field is therefore intimately linked with the coronal structure and evolution during the solar cycle. We summarize recent experimental results from active satellite experiments on Ulysses and the Advanced Composition Explorer (ACE). These results provide constraints on the sources of the solar wind and also the magnetic structure of the heliosphere and the corona. These results suggest the relevance of reconnection processes and differential rotation effects close to the Sun. This leads to large perturbations from a standard Archimedean spiral configuration which cannot be successfully modeled using coronal models which assume a potential magnetic field.

A comparison of solar wind streams and coronal structure near solar minimum

1977 ◽  
Vol 4 (7) ◽  
pp. 291-294 ◽  
Author(s):  
J. T. Nolte ◽  
J. M. Davis ◽  
M. Gerassimenko ◽  
A. J. Lazarus ◽  
J. D. Sullivan
Keyword(s):  
Solar Wind ◽  
Solar Minimum ◽  
Coronal Structure

High coronal structure of high velocity solar wind stream sources

Solar Physics ◽  
1977 ◽  
Vol 51 (2) ◽  
pp. 459-471 ◽  
Author(s):  
J. T. Nolte ◽  
A. S. Krieger ◽  
E. C. Roelof ◽  
R. E. Gold
Keyword(s):  
Solar Wind ◽  
High Velocity ◽  
Coronal Structure ◽  
Solar Wind Stream

Saturn's E, G and F rings: modulated by the plasma sheet

1984 ◽  
Vol 75 ◽  
pp. 597
Author(s):  
E. Grün ◽  
G.E. Morfill ◽  
T.V. Johnson ◽  
G.H. Schwehm
Keyword(s):  
Solar Wind ◽  
Direct Contact ◽  
Transport Processes ◽  
Time Variable ◽  
Dust Particles ◽  
Spatial Diffusion ◽  
Drag Forces ◽  
Orbit Perturbation ◽  
Time Variations ◽  
F Ring

ABSTRACTSaturn's broad E ring, the narrow G ring and the structured and apparently time variable F ring(s), contain many micron and sub-micron sized particles, which make up the “visible” component. These rings (or ring systems) are in direct contact with magnetospheric plasma. Fluctuations in the plasma density and/or mean energy, due to magnetospheric and solar wind processes, may induce stochastic charge variations on the dust particles, which in turn lead to an orbit perturbation and spatial diffusion. It is suggested that the extent of the E ring and the braided, kinky structure of certain portions of the F rings as well as possible time variations are a result of plasma induced electromagnetic perturbations and drag forces. The G ring, in this scenario, requires some form of shepherding and should be akin to the F ring in structure. Sputtering of micron-sized dust particles in the E ring by magnetospheric ions yields lifetimes of 102to 104years. This effect as well as the plasma induced transport processes require an active source for the E ring, probably Enceladus.

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