A View of Solar Magnetic Fields, the Solar Corona and the Solar Wind in Three Dimensions.
Abstract
In the last few years it was learned that the solar corona and the solar wind are three-dimensional. That is, the deviations from spherical or even cylindrical symmetry and first-order effects, that are important for our basic description and indeed physical understanding of the coronal expansion. The recognition of this simple fact has been a slow process; perhaps because it complicates the mathematical treatment. Even a quick look at the solar corona reveals a highly structured medium with large density gradients. It has long- almost for a century as a matter of fact (Bigelow, 1889)- been suggested that magnetic fields are the fundamental agent that controls the shape of the corona and determines the inner boundary conditions for the solar wind escape. Only recently have we recognized how dominant is the role of large-scale magnetic fields in determining the global structure of the solar wind. The highly successful 'SKYLAB Workshop on Coronal Holes' that was conducted last year has been important for the general acceptance of the new three-dimensional description of the structure of the corona and the interplanetary magnetic field. Zirker (1977) and Hundhausen (1977) have aptly summarized the insight resulting from this work. The present review will attempt a further synthesis based on a broader database than that available to the Workshop. We will attempt to provide a unified viewpoint recognizing that such an attempt is usually associated with a certain degree of oversimplification.
Document Details
- Document Type
- Technical Report
- Publication Date
- Jan 01, 1978
- Accession Number
- ADA086442
Entities
People
- John M. Wilcox
- Leif Svalgaard
Organizations
- Stanford University