Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

Solar Physics ◽  
1986 ◽  
Vol 105 (2) ◽  
Author(s):  
A.W. Hood
Keyword(s):  
Magnetic Fields ◽  
Coronal Magnetic Fields ◽  
Mhd Stability ◽  
Line Tying

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.

scholarly journals Boundary Fitting Problems Associated with Coronal Magnetic Models

1974 ◽  
Vol 57 ◽  
pp. 89-91 ◽  
Author(s):  
Kenneth H. Schatten
Keyword(s):  
Magnetic Fields ◽  
Legendre Polynomial ◽  
Magnetic Monopole ◽  
Polynomial Fit ◽  
Coronal Magnetic Fields ◽  
Boundary Fitting

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).

Thermal condensations in coronal magnetic fields

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

scholarly journals Distinguishing between coronal cloud prominences and channel prominences and their associations with solar and stellar flares

2015 ◽  
Vol 11 (S320) ◽  
pp. 278-287
Author(s):  
Sara F. Martin ◽  
Oddbjorn Engvold ◽  
Yong Lin ◽  
Jacqueline Alves da Silva
Keyword(s):  
Magnetic Fields ◽  
Sunspot Number ◽  
Maximum Height ◽  
Stellar Flares ◽  
Curved Trajectories ◽  
Coronal Magnetic Fields ◽  
Coronal Rain

AbstractTo better understand the differences between coronal cloud prominences and channel prominences, we systematically identified and analyzed coronal cloud prominences recorded in SDO/AIA images at 304 Å from 2010 May 20 through 2012 April 28. For the 225 cases identified, their numbers vary directly with the sunspot number. Their durations are typically less than 3 days. Their most frequent maximum height is 90,000 + and - 10,000 km. We offer our hypothesis that many coronal cloud prominences originate from some of the mass of previously erupted filaments ejected high out of their filament channels; subsequently part of this mass falls and collects in leaky magnetic troughs among coronal magnetic fields which constrain the leaked mass to slowly drain downward along curved trajectories where it appears as coronal rain. Currently there is inadequate evidence for a convincing correspondence between either coronal cloud prominences or channel prominences with stellar prominences detected to date.

Sign in / Sign up

Export Citation Format

Share Document