34th Solar Physics Division Meeting, June 2003
Session 4 Corona II
Poster, Monday, June 16, 2003, 3:30-5:00pm, Mezzanine

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[4.06] Hydrodynamic Simulations of Longitudinal Intensity Oscillations Observed in Coronal Loops by TRACE

S.E. Tanner, J.A. Klimchuk (Naval Research Lab), A.W. Hood, I. De Moortel (Univ. of St. Andrews)

Propagating intensity disturbances are often observed by TRACE in large coronal loops located at the perimeters of active regions (e.g., De Moortel et al., 2002, Solar Phys., 209, 61). On average, the disturbances have periods of 280 s, propagation speeds of 120 km s-1, intensity amplitudes of 4%, and surprisingly small damping (detection) lengths of 9000 km. In addition, there is a positive correlation between damping length and period. The preliminary interpretation of these disturbances is that they are rapidly dissipating slow magneto-acoustic waves.

To investigate this interpretation more rigorously, we have performed a series of detailed coronal loop simulations using our 1D hydrodynamic code, ARGOS. We generate waves in the loop by imposing a spatially localized oscillating force at the loop footpoint, using a range of different oscillation periods. We here report on the results of our study and, in particular, whether the damping lengths have the properties observed by TRACE.

This work was supported by NASA and ONR.

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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.