34th Solar Physics Division Meeting, June 2003
Session 1 Corona I
Oral, Monday, June 16, 2003, 9:00am-12:00noon, Auditorium

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[1.10] Propagating Disturbances in the Lower Solar Corona

M. J. Wills-Davey (Montana State University)

TRACE observations allow us to see propagating coronal waves in multiple narrowband filters and with high spatiotemporal resolution. We analyze an event from 13 June 1998, and determine from the morphology that it is a fast-mode MHD wave. We also analyze three other TRACE propagations and compare their morphology to the 13 June 1998 event.

By developing new mapping algorithms, we automate the tracking of propagating waves, finding reproducible fronts and natural trajectories, as well as fluxes and dissipation rates. Through comparison of EUV passbands, we place altitude and temperature constraints on the 13 June 1998 event, and show that the front moves through the lowest part of the corona. This analysis is reinforced analytically, by considering a propagating MHD wave in a hydrostatic atmosphere.

Conclusions offer explanations for the dearth of soft x-ray observations of propagating waves, as well as the seeming uniformity of EUV events. In light of the above-mentioned propagation constraints, the usefulness of such waves for coronal seismology is addressed.


The author(s) of this abstract have provided an email address for comments about the abstract: meredith@solar.physics.montana.edu

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