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Spectroscopic Studies of Solar Corona VI: Trend in Line-width Variation of Coronal Emission Lines with Height Independent of the Structure of Coronal Loops
Sun corona coronal structures emission line widt techniques spectroscopy
2010/9/16
We have obtained spectroscopic observations in coronal emission lines by choosing two lines simultaneously, one [Fe x] 6374Å and the other [Fe xi] 7892Å or [Fe xiii] 10747Å or [Fe xi...
Nanoflares and Heating of the Solar Corona
Sun stars—magnetic reconnection coronal heating—nanoflares
2010/9/16
Coronal heating by nanoflares is presented by using observational,analytical, numerical simulation and statistical results. Numerical simulations show the formation of numerous current sheets if the m...
MHD turbulence and heating of the open field-line solar corona
MHD turbulence open field-line solar corona
2009/11/11
This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static mag...
Intermittent heating of the solar corona by MHD turbulence
Intermittent heating solar corona MHD turbulence
2009/11/3
As the dissipation mechanisms considered for the heating of the solar corona would be sufficiently efficient only in the presence of small scales, turbulence is thought to be a key player in the coron...
Joule heating and anomalous resistivity in the solar corona
Joule heating anomalous resistivity solar corona
2009/10/30
Recent radioastronomical observations of Faraday rotation in the solar corona can be interpreted as evidence for coronal currents, with values as large as 2.5×109 Amperes (Spangler, 2007). These estim...
Spectroscopic Studies of Solar Corona VI：Trend in Line-width Variation of Coronal Emission Lines with Height Independent of the Structure of Coronal Loops
Sun:corona coronal structures emission line widths techniques:spectroscopy
2009/5/7
We have obtained spectroscopic observations in coronal emission lines by choosing two lines simultaneously, one [Fe x] 6374Å and the other [Fe xi] 7892Å or [Fe xiii] 10747Å or [Fe xiv] ...
Nanoflares and Heating of the Solar Corona
Sun:stars magnetic reconnection:coronal heating nanoflares
2009/5/7
Coronal heating by nanoflares is presented by using observational, analytical, numerical simulation and statistical results. Numerical simulations show the formation of numerous current sheets if the ...
MODELING STATIC MAGNETIC FIELD STRUCTURES IN SOLAR CORONA (Invited review)
Sun magnetic fields-Sun corona
2009/2/23
We give an overview of procedures to recover and simulate typical
coronal static magnetic field topologies from given boundary data on the photo-
sphere. Relatively simple analytical treatments allo...
Viscous Dissipation of Magnetosonic Waves in Solar Corona
magnetosonic waves solar corona dispersion relation damping length scale
2010/4/15
Wave propagation and dissipation of magnetosonic waves are considered in an inhomogenous viscous coronal plasma permeated by a spatially varying magnetic field. In the linear magnetohydrodynamic appro...