Volume 452, Number 3, June IV 2006
|Page(s)||1075 - 1082|
|Published online||06 June 2006|
Study of a transient siphon flow in a cold loop
Armagh Observatory, College Hill, Armagh BT61 9DG, Northerm Ireland e-mail: firstname.lastname@example.org
2 Solar Physics and Upper-Atmosphere Research Group, Department of Applied Mathematics, University of Sheffield, Sheffield, S3 7RH, UK
3 Solar Influences Data analysis Center, Royal Observatory of Belgium, 3 Circular Avenue, 1180 Brussels, Belgium
4 Space & Atmospheric Physics, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BZ, UK
Accepted: 26 February 2006
Context.The nature of loops is still a matter of debate with several explanations having been put forward. Simultaneous spectral and imaging data have the capacity to provide a new insight into mass motions, dynamics and energetics of loops.
Aims.We report on spectral data taken with the Solar Ultraviolet Measurements of Emitted Radiation spectrograph (SUMER) and imaging data from the Transition Region and Coronal Explorer (TRACE) of a transient event which occurred in a cold loop, lasting a few minutes.
Methods.A sequence of TRACE images in the 1550 Å and 171 Å filters show a disturbance which originated at one foot-point and propagates along the loop. The SUMER slit was placed at the other foot-point of the loop. In order to interpret the results, numerical simulations were performed with the results then converted into observable quantities and compared with the data.
Results.During the event a radiance increase and a relative red shift of was detected in the N v 1238.82 Å line. 1D numerical simulations are performed and observable quantities derived from the results of the simulations. The observed dynamic behaviour of the N v 1238.82 Å line profiles was recovered.
Conclusions.The results suggest that the observations could be interpreted in terms of a short-lived siphon flow reaching a speed of and driven by a nonlinear heating pulse. The energies required to drive the observed red-shifts are estimated to be about 1025 erg. The absence of a significant blue-shift caused by the return flow is explained.
Key words: Sun: corona / Sun: transition region / line: profiles / methods: observational / methods: numerical / hydrodynamics
© ESO, 2006
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