๐”– Bobbio Scriptorium
โœฆ   LIBER   โœฆ

The shape of twisted, line-tied coronal loops

โœ Scribed by P. K. Browning; A. W. Hood


Publisher
Springer
Year
1989
Tongue
English
Weight
897 KB
Volume
124
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.


๐Ÿ“œ SIMILAR VOLUMES


The evolution of twisted coronal loops
โœ J. A. Robertson; A. W. Hood; R. M. Lothian ๐Ÿ“‚ Article ๐Ÿ“… 1992 ๐Ÿ› Springer ๐ŸŒ English โš– 815 KB

The evolution of coronal loops in response to slow photospheric twisting motions is investigated using a variety of methods. Firstly, by solving the time-dependent equations it is shown that the field essentially evolves through a sequence of 2-D equilibria with no evidence of rapid dynamic evolutio

The shape of buoyant coronal loops in a
โœ P. K. Browning; E. R. Priest ๐Ÿ“‚ Article ๐Ÿ“… 1986 ๐Ÿ› Springer ๐ŸŒ English โš– 840 KB

The equilibrium and non-equilibrium properties of a coronal loop embedded in a stratified isothermal atmosphere are investigated. The shape of the loop is determined by a balance between magnetic tension, buoyancy, and external pressure gradients. The footpoints of the loop are anchored in the photo

The structure of coronal magnetic loops
โœ Riccardo Giachetti; Gerard Hoven; Claudio Chiuderi ๐Ÿ“‚ Article ๐Ÿ“… 1977 ๐Ÿ› Springer ๐ŸŒ English โš– 846 KB
The thermal statics of coronal loops
โœ B. Roberts; S. Frankenthal ๐Ÿ“‚ Article ๐Ÿ“… 1980 ๐Ÿ› Springer ๐ŸŒ English โš– 394 KB

The thermal statics of constant pressure coronal loops is discussed, with particular emphasis on non-equilibrium and scaling relations. An analytical solution showing explicitly the occurrence of non-equilibrium in radiation dominated loops is presented. In addition, the general scaling law for hot

The structure of coronal magnetic loops
โœ Claudio Chiuderi; Riccardo Giachetti; Gerard Hoven ๐Ÿ“‚ Article ๐Ÿ“… 1977 ๐Ÿ› Springer ๐ŸŒ English โš– 958 KB

We present here a model, based on observations, for the magnetic-field equilibrium of a cool coronal loop. The pressure structure, taken from the Harvard/Skylab EUV data, is used to modify the usual force-free-field form in quasi-cylindrical symmetry. The resulting field, which has the same directio