Physics
Scientific paper
Feb 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...90..315s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 90, Feb. 1984, p. 315-324.
Physics
4
Emission Spectra, Magnetohydrodynamic Waves, Solar Corona, Solar Prominences, Visible Spectrum, Coronagraphs, Extreme Ultraviolet Radiation, Image Analysis, Solar Magnetic Field
Scientific paper
Emission-line coronagraph images of a high-latitude, nominally quiescent prominence, recorded at wavelengths of H-alpha, 6374 A(Fe X) and 5303 A (Fe XIV), are analyzed. Over a two-day period, the coronal images, which are found to arise predominantly from coronal emission, evolve such that the emission becomes concentrated at locations corresponding to the outer regions of the prominence. This edge enhancement has similar characteristics to results inferred from EUV prominence observations. It is postulated that this coronal emission associated with the prominence results from MHD wave dissipation. Dissipation lengths for slow-mode, fast-mode and Alfven waves are estimated for different prominence conditions. Of these, fast-mode waves appear to be the most physically realistic heating source if the prominence magnetic field is along the length of the prominence.
Smartt Raymond N.
Zhang Zhongsheng
No associations
LandOfFree
Visible coronal emission associated with a quiescent prominence does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Visible coronal emission associated with a quiescent prominence, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Visible coronal emission associated with a quiescent prominence will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1859421