Abstract:
We studied a blowout jet that occurred at the west limb of the Sun on 2014 August 29 using high-resolution
imaging/spectroscopic observations provided by the Solar Dynamics Observatory/Atmospheric Imaging
Assembly and the Interface Region Imaging Spectrograph. An inverse γ-shaped flux rope appeared before the
jet–morphological indication of the onset of kink instability. The twisted field lines of the kink-unstable flux rope
reconnected at its bright knot and launched the blowout jet at ≈06:30:43 UT with an average speed of 234 km s−1
.Just after the launch, the northern leg of the flux rope erupted completely. The time–distance diagrams show
multiple spikes or bright dots, which is the result of periodic fluctuations, i.e., quasi-periodic fluctuations (QPPs).
The wavelet analysis confirms that QPPs have a dominant period of ≈3 minutes. IRIS spectra (Si IV, C II, and
Mg II) may also indicate the occurrence of magnetic reconnection through the existence of broad and complex
profiles and bidirectional flows in the jet. Further, we found that line broadening is periodic with a period of ≈3
minutes, and plasma upflow always occurs when the line width is high, i.e., multiple reconnection may produce
periodic line broadening. The emission measure (EM) curves also show the same period of ≈3 minutes in different
temperature bins. The images and EM show that this jet spire is mainly cool (chromospheric/transition region)
rather than hot (coronal) material. Further, line broadening, intensity, and EM curves have a period of ≈3 minutes,
which strongly supports the fact that multiple magnetic reconnection triggers QPPs in the blowout jet.
