Astronomy & Space Science · AST-137
Sunspots & Solar Magnetism: Structures & Vocabulary
A source-linked chapter designed to teach the subject itself, not a generic lesson template.
Chapter map
Follow the actual ideas in this lesson.
The sequence below comes from this topic's published material. Sections expand or contract with the subject instead of forcing every lesson into the same five-step mold.
Structure
Components and relationships in Sunspots & Solar Magnetism
Sunspots often occur in magnetically linked groups with umbrae and penumbrae. The visible sunspot count rises and falls over an average cycle near 11 years, while magnetic polarity reversals make the full magnetic cycle about 22 years. The Sun also rotates differentially, with the equator rotating faster than higher latitudes.
Chapter review
Assessment still in review.
The chapter is published, but its assessment has not completed the verification and QA pipeline yet. It will appear here after publication.
References & evidence
Source library for this chapter
These are the linked sources supporting the verified claims used throughout the lesson.
- 01The Solar CycleOpen source ↗
OpenStax Astronomy 2e
View claim-by-claim traceability3 verified claims
The Sun's electrically conducting plasma and differential rotation stretch, shear, and regenerate magnetic fields through dynamo processes.
supported · checked Sep 22, 2026Sunspots are relatively cool, dark regions of the photosphere associated with intense magnetic fields.
supported · checked Sep 22, 2026Spectropolarimetric observations measure strong magnetic fields in sunspots, and the Zeeman effect splits spectral lines in proportion to field strength.
supported · checked Sep 22, 2026