| Issue |
A&A
Volume 542, June 2012
|
|
|---|---|---|
| Article Number | A70 | |
| Number of page(s) | 9 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361/201117218 | |
| Published online | 08 June 2012 | |
Observations of quasi-periodic phenomena associated with a large blowout solar jet⋆
1 Solar Physics and Space Plasma Research Centre (SP 2RC), University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK
e-mail: r.j.morton@sheffield.ac.uk; robertus@sheffield.ac.uk
2 Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263129, India
Received: 9 May 2011
Accepted: 20 April 2012
Aims. A variety of periodic phenomena have been observed in conjunction with large solar jets. We aim to find further evidence for (quasi-)periodic behaviour in solar jets and determine what the periodic behaviour can tell us about the excitation mechanism and formation process of the large solar jet.
Methods. Using the 304 Å (He-II), 171 Å (Fe IX), 193 Å (Fe XII/XXIV) and 131 Å (Fe VIII/XXI) filters onboard the Solar Dynamic Observatory (SDO) Atmospheric Imaging Assembly (AIA), we investigate the intensity oscillations associated with a solar jet.
Results. Evidence is provided for multiple magnetic reconnection events occurring between a pre-twisted, closed field and open field lines. Components of the jet are seen in multiple SDO/AIA filters covering a wide range of temperatures, suggesting the jet can be classified as a blowout jet. Two bright, elongated features are observed to be co-spatial with the large jet, appearing at the jet’s footpoints. Investigation of these features reveal they are defined by multiple plasma ejections. The ejecta display (quasi-)periodic behaviour on timescales of 50 s and have rise velocities of 40–150 km s-1 along the open field lines. Due to the suggestion that the large jet is reconnection-driven and the observed properties of the ejecta, we further propose that these ejecta events are similar to type-II spicules. The bright features also display (quasi)-periodic intensity perturbations on the timescale of 300 s. Possible explanations for the existence of the (quasi-)periodic perturbations in terms of jet dynamics and the response of the transition region are discussed.
Key words: magnetohydrodynamics (MHD) / waves / Sun: oscillations / Sun: atmosphere
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© ESO, 2012
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