Abstract
We address the origin of the patchy dark and bright emission structure, known as moss, observed by TRACE extreme ultraviolet observations of the solar disk. Here we propose an explanation based on turbulent, patchy heat conduction from the corona into the transition region. Computer simulations demonstrate that magnetic turbulence in coronal loops develops a flux rope structure with current sheets near the flux rope boundaries. Localized heating due to current sheet activity such as magnetic reconnection is followed by heat conduction along turbulent magnetic field lines. The field line trajectories tend to remain near the flux rope boundaries, resulting in selective heating of the plasma in the transition region. This can explain the network of bright regions in the observed moss morphology.
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.
