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Abstract:
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The Sun's corona is made up of hot plasma, typically at 1--2 million K. The corona is organized on large scales by the magnetic field of the Sun. Because the plasma is highly ionized, it forms loops tracing the field lines. The plasma cools by emitting high energy X-ray and EUV radiation, which is detected with the aid of orbiting solar telescopes. The detection and characterization of coronal loops thus leads to constraints on the magnetic and energetic environment on the Sun. However, coronal loops are notoriously difficult to extract from images because they overlap and form low-contrast images. Thus far, astronomers have depended upon visual inspection for the identification of interesting features. We have now implemented a morphological analysis process to identify and extract loop segments, and subsequently to model the coronal magnetic field using them. [NASA/LWSTRT:NNGO5GM44G]
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