Magnetic fields and the temperature structure of the chromosphere-corona interface

✍ Scribed by Roger A. Kopp; Max Kuperus

• Publisher: Springer
• Year: 1968
• Tongue: English
• Weight: 742 KB
• Volume: 4
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00148082

✦ Synopsis

The temperature structure of the transition region between the chromosphere and corona is discussed in the context of current ideas about magnetic fields in these layers. Magnetic channeling of the downward conductive heat flow from the corona into the regions of enhanced field at the supergranulation boundaries is proposed as a mechanism for explaining the measured intensities of solar ultraviolet emission lines which originate in layers with temperatures below 105 ~ It is shown that nearly all of the observed ultraviolet line emission originates in interspicule regions, and that this emission plays an important part in the energy balance of the cooler layers of the transition region. It is suggested that certain motions observed in the upper chromosphere may represent the earliest visual evidence for conversion of inftowing conduction energy into kinetic motions. * On leave from the Observatory 'Sonnenborgh' at Utrecht, The Netherlands.