Automatic Detection of Coronal Loops from SDO-AIA Data
Abstract
Heliophysicists have searched for an explanation to the coronal heating problem since the 1940's. The Sun's atmosphere averages one million Kelvin, while its surface is a mere 6000K. Coronal loops form when hot plasma travels along closed magnetic flux tubes. The evolution of Extreme Ultraviolet (EUV) coronal loops has been studied for many years and the question is how these loops are being heated. The evolution of loops give clue to the coronal heating mechanism (Mulu-Moore, et al. 2011). The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) provides a special opportunity to observe, analyze, and differentiate the loop properties and derive important constraints to the coronal heating mechanism. In this project we used evolution to identify and extract loop pixels from cubes of AIA data.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2012
- Bibcode:
- 2012AGUFMSH13A2240O
- Keywords:
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- 7500 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7509 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY / Corona;
- 7524 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY / Magnetic fields;
- 7800 SPACE PLASMA PHYSICS