Abstract
Yohkoh X-ray images of the Sun show ubiquitous bright loops. Most of the analyses of Yohkoh data so far made on the temperature structure of the coronal loops concentrated on the individual X-ray loops. We, however, need to remember that the high temperature corona apparently exists outside the distinct loops and in the diffuse region. The fundamental questions in the context of coronal heating are why specific magnetic structures are bright in X-rays and what the difference is between bright X-ray loops and faint diffuse regions. As a first step to answer these questions observationally, we obtain high-quality temperature maps of the entire active regions from X-ray maps summed over a certain time interval by sacrificing the time resolution.
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T. Yoshida and S. Tsuneta, (1996), ApJ, 459, 342
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© 1996 Kluwer Academic Publishers
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Yoshida, T., Tsuneta, S. (1996). Temperature Structure of Solar Active Regions. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_7
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DOI: https://doi.org/10.1007/978-94-009-0315-9_7
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