The topological structure of the coronal-interplanetary magnetic field is determined by the arrangement of the neutral lines at the coronal base. It is characterized by nested separatrices, which are interfaces between closed and open field lines or between oppositely directed open field lines, in t
A model of interplanetary and coronal magnetic fields
โ Scribed by Kenneth H. Schatten; John M. Wilcox; Norman F. Ness
- Publisher
- Springer
- Year
- 1969
- Tongue
- English
- Weight
- 705 KB
- Volume
- 6
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
โฆ Synopsis
A model of the large-scale magnetic field structure above the photosphere uses a Green's function solution to Maxwell's equations. Sources for the magnetic field are related to the observed photospheric field and to the field computed at a 'source' surface about 0.6 R G above the photosphere. The large-scale interplanetary magnetic field sector pattern is related to the field pattern at this 'source' surface. The model generates magnetic field patterns on the 'source' surface that compare well with interplanetary observations. Comparisons are shown with observations of the interplanetary magnetic field obtained by the IMP-3 satellite.
๐ SIMILAR VOLUMES
The observational evidence on the strength of the coronal magnetic field above active regions is reviewed. Recent advances in observations and plasma theory are used to determine which data are the more reliable and to revise some earlier estimates of field strength. The results from the different t
A long-standing misconception about the mathematical validity of utilizing Green's function solutions to coronal magnetic fields is discussed. Although this type of solution does not fit the observed line-of-sight component of the photospheric magnetic field, but rather the net flux in a region, the