Helmet Streamers Gone Unstable: Two‐Fluid Magnetohydrodynamic Models of the Solar Corona

2004 ◽  
Vol 603 (1) ◽  
pp. 307-321 ◽  
Author(s):  
Eirik Endeve ◽  
Thomas E. Holzer ◽  
Egil Leer
Keyword(s):  
Solar Corona ◽  
Magnetohydrodynamic Models ◽  
Two Fluid

scholarly journals Two-fluid model of the solar corona

Solar Physics ◽  
1974 ◽  
Vol 37 (1) ◽  
pp. 183-187 ◽  
Author(s):  
J. W. Knight ◽  
C. E. Newman ◽  
P. A. Sturrock
Keyword(s):  
Solar Corona ◽  
Fluid Model ◽  
Two Fluid Model ◽  
Two Fluid

scholarly journals Two-fluid and magnetohydrodynamic modelling of magnetic reconnection in the MAST spherical tokamak and the solar corona

2015 ◽  
Vol 58 (1) ◽  
pp. 014041 ◽  
Author(s):  
P K Browning ◽  
S Cardnell ◽  
M Evans ◽  
F Arese Lucini ◽  
V S Lukin ◽  
...  
Keyword(s):  
Solar Corona ◽  
Magnetic Reconnection ◽  
Spherical Tokamak ◽  
Two Fluid

Validation of single-fluid and two-fluid magnetohydrodynamic models of the helicity injected torus spheromak experiment with the NIMROD code

2013 ◽  
Vol 20 (8) ◽  
pp. 082512 ◽  
Author(s):  
Cihan Akcay ◽  
Charlson C. Kim ◽  
Brian S. Victor ◽  
Thomas R. Jarboe
Keyword(s):  
Magnetohydrodynamic Models ◽  
Two Fluid

Reply to billings concerning ?Two-Fluid Model of the Solar Corona?

Solar Physics ◽  
1975 ◽  
Vol 41 (2) ◽  
pp. 371-371
Author(s):  
J. W. Knight ◽  
C. E. Newman ◽  
P. A. Sturrock
Keyword(s):  
Solar Corona ◽  
Fluid Model ◽  
Two Fluid Model ◽  
Two Fluid

Colour Photometry of the Solar Corona of July 11, 1991

1994 ◽  
Vol 144 ◽  
pp. 597-599 ◽  
Author(s):  
I. V. Alexeyeva ◽  
N. L. Kroussanova ◽  
M. V. Streltsova
Keyword(s):  
Solar Corona ◽  
Red Emission ◽  
Coronal Structures

AbstractThe results of photometry of colour positives of the solar corona of July 11, 1991 are presented. Observations of the white corona were made without radial niters in Jojutla (Mexico). Dependences of coronal brightness on distance in the red (640 nm) and blue (420 nm) wavelength intervals are deduced for different coronal structures up to 3.0-3.5R⊙. The effect of ”reddening“ is noted. The excess of the red emission to the blue one (I640nm/I420nm) is found to be 1.20 and 1.17 at distance of 2.2R⊙for the N-E helmet streamer (P ≃ 37°) and the N-W region of low brightness (P ≃ 339°), respectively.

July 11, 1991 Eclipse Corona Photometry by the Results of Electropolarimetric and CCD-Matrix Observations

1994 ◽  
Vol 144 ◽  
pp. 567-569
Author(s):  
V. Kulidzanishvili ◽  
D. Georgobiani
Keyword(s):  
Solar Corona ◽  
Observational Data ◽  
Solar Limb ◽  
Ccd Matrix

AbstractThe observational data of July 11, 1991 eclipse solar corona obtained by both electropolarimeter (EP) and CCD-matrix were processed. Using these data, the solar corona photometry was carried out. The results of EP data are compared with the ones of CCD data. It must be noted here that the CCD data give us only characteristics of the inner corona, while the EP data show the features of both the inner and middle corona up to 4R⊙. Standard flattening indexϵis evaluated from both data. The dependence of the flattening index on the distance from the solar limb is investigated. The isophotes in Na and Ca lines are plotted. Based on these data some ideas and conclusions on the type of the solar corona are presented.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

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