| タイトル | Structure and Dynamics of the Solar Corona |
| 本文（外部サイト） | http://hdl.handle.net/2060/19950007169 |
| 著者（英） | Schnack, D. D. |
| 著者所属（英） | Science Applications, Inc. |
| 発行日 | 1994-10-19 |
| 言語 | eng |
| 内容記述 | Advanced computational techniques were used to study solar coronal heating and coronal mass ejections. A three dimensional, time dependent resistive magnetohydrodynamic code was used to study the dynamic response of a model corona to continuous, slow, random magnetic footpoint displacements in the photosphere. Three dimensional numerical simulations of the response of the corona to simple smooth braiding flows in the photosphere were calculated to illustrate and understand the spontaneous formation of current filaments. Two dimensional steady state helmet streamer configurations were obtained by determining the time asymptotic state of the interaction of an initially one dimensinal transponic solar wind with a spherical potential dipole field. The disruption of the steady state helmet streamer configuration was studied as a response to shearing of the magnetic footpoints of the closed field lines under the helmet. |
| NASA分類 | SOLAR PHYSICS |
| レポートNO | 95N13582
NASA-CR-196978
NAS 1.26:196978
SAIC-94/1151 |
| 権利 | No Copyright |
|
