Non-Linear Evolution of Erupting Coronal Magnetic Fields

Author(s):  
Bambang Setiahadi ◽  
Bachtiar Anwar ◽  
Maki Akioka ◽  
Takashi Sakurai
1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora

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.


1974 ◽  
Vol 57 ◽  
pp. 89-91 ◽  
Author(s):  
Kenneth H. Schatten

The calculation of coronal magnetic fields was first suggested by Gold (1958). Altschuler and Newkirk (1969) and Newkirk et al. (1968) used a Legendre polynomial fit to the photospheric observations of magnetic fields whereas Schatten (1968) with Wilcox and Ness (Schatten et al., 1969) use a magnetic monopole fit, first incorporated by Schmidt (1964).


2000 ◽  
Vol 18 (3) ◽  
pp. 519-534 ◽  
Author(s):  
F. Gillet ◽  
O. Pierre-Louis ◽  
C. Misbah

Solar Physics ◽  
1988 ◽  
Vol 115 (1) ◽  
pp. 61-80 ◽  
Author(s):  
A. Hood ◽  
U. Anzer

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