Observational evidence of underlying driving of longitudinal oscillations in coronal loops

Details Observational evidence of underlying driving of longitudinal oscillations in coronal loops Observational evidence of underlying driving of longitudinal oscillations in coronal loops

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..211d&link_type=abstract

In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun

Physics

Sun, Corona, Oscillations

Scientific paper

We give an overview of both geometric and physical parameters of propagating disturbances in coronal loops, using high cadence TRACE data (JOP83 & JOP144). The majority of these outward propagating oscillations are found in the footpoints of large diffuse coronal loop structures, close to active regions. The disturbances travel outward with a propagation speed v = 122±43 km s-1. The variations in intensity are estimated to be of the order of 4.1±1.5%, compared to the background brightness and are found to be damped very quickly, within 8.9±4.4 Mm along the loop. Using a wavelet analysis, periods in the 282±93 seconds range are obtained. However, it was found that loops that are situated above sunspot regions display intensity oscillations with a period smaller than 200 seconds, whereas oscillations in 'non-sunspot' loops show periods larger than 200 seconds. This result provides evidence that the underlying oscillations can propagate through the transition region and into the corona. We conclude that the observed longitudinal oscillations are not flare-driven but are most likely caused by an underlying driver exciting the loop footpoints.

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