Abstract
The discovery of coronal loops has provoked major revisions in the theory of solar and stellar atmospheres. The solar corona is now recognized as a highly structured plasma, organized by bundles of intense magnetic field into individual arch- and loop-like structures along which gas can flow1. Each arch, rooted in the solar interior, extends through the chromosphere (T 106Κ) in its upper reaches. Early attempts at explaining the temperature and density structure of isolated static loops met with considerable success, despite the simplicity of the theory2,3; however, attempts to generalize the theory to describe loops with mass flows have remained singularly unsuccessful4–9. Here we point out that the puzzling observational properties of loop mass flows10–15 can be naturally explained if the loop is sufficiently cool (T ≲ 106 K)—that is, if it contains no coronal plasma.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
