Rotating Network Jets in the quiet Sun as Observed by IRIS
P. Kayshap, K. Murawski, A.K. Srivastava, B.N. Dwivedi

TL;DR
This study provides a detailed observational analysis of rotating network jets in the quiet Sun, revealing their kinematics, rotational motion, and likely formation mechanism through high-resolution IRIS and SDO data.
Contribution
It is the first to report the omnipresent rotational motion of network jets and links their formation to magnetic reconnection.
Findings
Mean jet speed is 140 km/s.
Jets exhibit inherited rotational motion with an average rotational velocity of 49.56 km/s.
Rotational motion is a key characteristic of network jets.
Abstract
Aims. We perform a detailed observational analysis of network jets to understand their kinematics, rotational motion and underlying triggering mechanism(s). We have analyzed the quiet-Sun (QS) data. Methods. IRIS high resolution imaging and spectral observations (SJI: Si iv 1400.0 \AA, Raster: Si iv 1393.75 \AA) are used to analyze the omnipresent rotating network jets in the transition-region (TR). In addition, we have also used Atmospheric Imaging Assembly (AIA) onboard Solar Dynamic Observation (SDO) observations. Results. The statistical analysis of fifty-one network jets is performed to understand various their mean properties, e.g., apparent speed (140.16+/-39.41 km/s), length (3.16+/-1.18 Mm), lifetimes (105.49+/-51.75 s). The Si iv 1393.75 \AA line has secondary component along with its main Gaussian, which is formed due to the high-speed plasma flows (i.e., network jets). The…
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