Abstract
The Sun is enveloped in a thick atmosphere which can be divided into the following three layers. As the lowest part, the photosphere has a thickness of only about 500 km. Above it is the chromosphere with a thickness of approximately 20,000 km. The outmost part is the corona, which has a scope of several to ten more solar radii. Its shape is not fixed and varies with the phase of the solar activity cycle. The magnetic field pervades the whole solar atmosphere and plays an important role in its structure, dynamics and evolution.
One of the key problems of solar physics is the question of the fine structure of the magnetic field. A. B. Severny, Some Problems of the Physics of the Sun (1988).
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
Author information
Authors and Affiliations
Rights and permissions
Copyright information
© 1994 Springer Science+Business Media Dordrecht
About this chapter
Cite this chapter
Shi-Hui, Y. (1994). Magnetic Fields of the Solar Atmosphere. In: Magnetic Fields of Celestial Bodies. Astrophysics and Space Science Library, vol 198. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0944-4_6
Download citation
DOI: https://doi.org/10.1007/978-94-011-0944-4_6
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-4407-3
Online ISBN: 978-94-011-0944-4
eBook Packages: Springer Book Archive