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Coronal loop information


Typical coronal loops observed by TRACE
Dynamics of coronal loops observed by SDO

In solar physics, a coronal loop is a well-defined arch-like structure in the Sun's atmosphere made up of relatively dense plasma confined and isolated from the surrounding medium by magnetic flux tubes. Coronal loops begin and end at two footpoints on the photosphere and project into the transition region and lower corona. They typically form and dissipate over periods of seconds to days[1] and may span anywhere from 1 to 1,000 megametres (621 to 621,000 mi) in length.[2]

Coronal loops are often associated with the strong magnetic fields located within active regions and sunspots. The number of coronal loops varies with the 11 year solar cycle.

  1. ^ Loff, Sarah (2015-04-17). "Coronal Loops in an Active Region of the Sun". NASA. Retrieved 2022-03-28.
  2. ^ Reale, Fabio (July 2014). "Coronal Loops: Observations and Modeling of Confined Plasma" (PDF). Living Reviews in Solar Physics. 11 (4): 4. Bibcode:2014LRSP...11....4R. doi:10.12942/lrsp-2014-4. PMC 4841190. PMID 27194957. Retrieved 16 March 2022.

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