Abstract
The jet on September 30, 1998, is part of a complex event that involved also other eruptive phenomena. Changes in the coronal magnetic field topology were observed during the ejection of the jet, as deduced from the Fe XIV green line emission. The whole event was well observed by both the H‐Alpha Solar Telescope for Argentina (HASTA) and the Mirror Coronagraph for Argentina (MICA), which are installed in the German‐Argentinean Solar Observatory at El Leoncito, Argentina. The Soft X‐ray Telescope (SXT) on board Yohkoh also observed the jet. In this work, observations of the first part of this complex event showing the evolution of the jet and release of blobs are presented. Certain features observed are interpreted as signatures of a magnetic reconnection process in the region. We conclude that existing theoretical and phenomenological models based on magnetic reconnection mechanisms could explain our observations, which span three temperature regimes far apart from each other.
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