Filament formation due to photospheric shear

Details Filament formation due to photospheric shear Filament formation due to photospheric shear

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442...47w&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 47-50 (SEE N87-20871 13-92)

Other

Magnetic Field Configurations, Magnetohydrodynamics, Photosphere, Plasma Density, Plasmas (Physics), Simulation, Solar Atmosphere, Solar Magnetic Field, Solar Physics, Solar Prominences, Solar Temperature, Sun, Evolution (Development), Isotherms, Line Spectra, Mathematical Models, Topography

Scientific paper

Recently, Wu et al. (1983, 1986) developed a three-dimensional, time-dependent axisymmetric ideal magnetohydrodynamic (MHD) model which has been used to study lower solar atmospheric response due to photospheric motion. They have shown that various observed solar features can be formed from these numerical simulation experiments. Some work currently in progress which has resulted from a specific numerical simulation experiment is reported. These results may elucidate the possible physical mechanism of formation of filament.

Affiliated with

Also associated with

No associations

Rating

Filament formation due to photospheric shear does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Filament formation due to photospheric shear, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Filament formation due to photospheric shear will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1126755