NASA Logo, External Link
Facebook icon, External Link to NASA STI page on Facebook Twitter icon, External Link to NASA STI on Twitter YouTube icon, External Link to NASA STI Channel on YouTube RSS icon, External Link to New NASA STI RSS Feed AddThis share icon
 

Record Details

Record 1 of 28705
Large-Scale Coronal Heating from "Cool" Activity in the Solar Magnetic Network
Author and Affiliation:
Falconer, D. A.(NASA Marshall Space Flight Center, Huntsville, AL United States)
Moore, R. L.(NASA Marshall Space Flight Center, Huntsville, AL United States)
Porter, J. G.(NASA Marshall Space Flight Center, Huntsville, AL United States)
Hathaway, D. H.(NASA Marshall Space Flight Center, Huntsville, AL United States)
Abstract: In Fe XII images from SOHO/EIT, the quiet solar corona shows structure on scales ranging from sub-supergranular (i.e., bright points and coronal network) to multi-supergranular (large-scale corona). In Falconer et al 1998 (Ap.J., 501, 386) we suppressed the large-scale background and found that the network-scale features are predominantly rooted in the magnetic network lanes at the boundaries of the supergranules. Taken together, the coronal network emission and bright point emission are only about 5% of the entire quiet solar coronal Fe XII emission. Here we investigate the relationship between the large-scale corona and the network as seen in three different EIT filters (He II, Fe IX-X, and Fe XII). Using the median-brightness contour, we divide the large-scale Fe XII corona into dim and bright halves, and find that the bright-half/dim half brightness ratio is about 1.5. We also find that the bright half relative to the dim half has 10 times greater total bright point Fe XII emission, 3 times greater Fe XII network emission, 2 times greater Fe IX-X network emission, 1.3 times greater He II network emission, and has 1.5 times more magnetic flux. Also, the cooler network (He II) radiates an order of magnitude more energy than the hotter coronal network (Fe IX-X, and Fe XII). From these results we infer that: 1) The heating of the network and the heating of the large-scale corona each increase roughly linearly with the underlying magnetic flux. 2) The production of network coronal bright points and heating of the coronal network each increase nonlinearly with the magnetic flux. 3) The heating of the large-scale corona is driven by widespread cooler network activity rather than by the exceptional network activity that produces the network coronal bright points and the coronal network. 4) The large-scale corona is heated by a nonthermal process since the driver of its heating is cooler than it is. This work was funded by the Solar Physics Branch of NASA's office of Space Science through the SR&T Program and the SEC Guest Investigator Program.
Publication Date: Jan 01, 1999
Document ID:
19990106580
(Acquired Nov 19, 1999)
Subject Category: SOLAR PHYSICS
Document Type: Conference Paper
Meeting Information: 13 Dec. 1999; San Francisco, CA; United States
Meeting Sponsor: American Geophysical Union; United States
Financial Sponsor: NASA Marshall Space Flight Center; Huntsville, AL United States
Organization Source: NASA Marshall Space Flight Center; Huntsville, AL United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: No Copyright
NASA Terms: SOLAR CORONA; SOLAR PHYSICS; SOLAR HEATING; SOHO MISSION; BRIGHTNESS; MAGNETIC FLUX; IRON; EMISSION SPECTRA
Availability Source: Other Sources
Availability Notes: Abstract Only;
› Back to Top
Find Similar Records
NASA Logo, External Link
NASA Official: Gerald Steeman
Site Curator: STI Program
Last Modified: August 22, 2011
Contact Us