Journal
SOLAR PHYSICS
Volume 246, Issue 1, Pages 53-63Publisher
SPRINGER
DOI: 10.1007/s11207-007-0392-6
Keywords
MHD : oscillations; corona; activity
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Funding
- STFC [PP/E001122/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E001122/1] Funding Source: researchfish
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High-cadence TRACE observations show that outward-propagating intensity disturbances are a common feature in large, quiescent coronal loops. Analysis of the frequency distribution of these modes shows peaks at both three- and five-minute periods, indicating that they may be driven by the solar surface oscillations (p modes). The energy flux contained within the coronal intensity disturbances is of the order of (1.1 +/- 0.4) x 10(3) ergs cm(-2)s(-1). A simple order-of-magnitude estimate of the damping rate of the relevant p modes allows us to put an observational constraint on the damping of p modes and shows that leakage into the overlying coronal atmosphere might be able to account for a significant fraction of p-mode damping.
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