HR: 17:15h
AN: SH24A-06    [Abstracts]
TI: Coronal Seismology and the Propagation of Acoustic Waves Along Coronal Loops
AU: * Klimchuk, J A
EM: klimchuk@nrl.navy.mil
AF: Naval Research Lab, 4555 Overlook Ave., SW, Washington, DC 20375 United States
AU: Tanner, S E
EM: sarah@godzilla.nrl.navy.mil
AF: Naval Research Lab, 4555 Overlook Ave., SW, Washington, DC 20375 United States
AU: De Moortel, I
EM: ineke@mcs.st-and.ac.uk
AF: School of Math and Statistics, University of St. Andrews, St. Andrews, KY16 9SS United Kingdom
AB: We use a combination of analytical theory, numerical simulation, and data analysis to study the propagation of acoustic waves along coronal loops. We show that the intensity perturbation of a wave depends on a number of factors, including dissipation of the wave energy, pressure and temperature gradients in the loop atmosphere, work action between the wave and a flow, and the sensitivity properties of the observing instrument. In particular, the scale length of the intensity perturbation varies directly with the dissipation scale length (i.e., damping length) and the scale lengths of pressure, temperature, and velocity. We simulate wave propagation in three different equilibrium loop models and find that dissipation and pressure and temperature stratification are the most important effects in the low corona where the waves are most easily detected. Velocity effects are small, and cross-sectional area variations play no direct role for lines-of-sight that are normal to the loop axis. The intensity perturbation scale lengths in our simulations agree very well with the scale lengths we measure in a sample of loops observed by {\it TRACE}. The median observed value is $4.35\times10^9$ cm. In some cases the intensity perturbation increases with height, which is likely an indication of a temperature inversion in the loop (i.e., temperature that decreases with height). Our most important conclusion is that thermal conduction, the primary damping mechanism, is accurately described by classical transport theory. There is no need to invoke anomalous processes to explain the observations.
DE: 7509 Corona
DE: 7549 Ultraviolet emissions
DE: 7594 Instruments and techniques
DE: 7859 Transport processes
DE: 7871 Waves and instabilities
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting