Waves in Solar Coronal Loops
Abstract
The corona is visible in the optical band only during a total solar eclipse or with a coronagraph. Coronal loops are believed to be plasma-filled closed magnetic flux anchored in the photosphere. Based on the temperature regime, they are generally classified into cool, warm, and hot loops. The magnetized coronal structures support propagation of various types of magnetohydrodynamics (MHD) waves. This chapter reviews the recent progress made in studies based on observations of four types of wave phenomena mainly occurring in coronal loops of active regions, including: flare-excited slow-mode waves; impulsively excited kink-mode waves; propagating slow magnetoacoustic waves; and ubiquitous propagating kink (Alfvénic) waves. This review not only comprehensively discusses these waves and coronal seismology but also topics that are newly emerging or hotly debated in order to provide the reader with useful guidance on further studies.
- Publication:
-
Geophysical Monograph Series
- Pub Date:
- February 2016
- DOI:
- 10.1002/9781119055006.ch23
- arXiv:
- arXiv:1803.11329
- Bibcode:
- 2016GMS...216..395W
- Keywords:
-
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 24 pages, 6 figures, published in 2016