Multiwavelength Study of on-disk Coronal Hole Jets with IRIS and SDO observations

TL;DR

This study uses IRIS and SDO observations to analyze two small-scale on-disk coronal hole jets, revealing their plasma properties, dynamics, and thermal structures, and highlighting differences in their evolution.

Contribution

It provides a detailed multiwavelength analysis of coronal hole jets, combining spectral and imaging data to characterize their plasma conditions and dynamics for the first time.

Findings

Both jets have high densities (~10^11 cm^-3) at their bases.

Spectral analysis shows two components indicating background and jet-related plasma.

Jets exhibit multithermal plasma distributions.

Abstract

Solar jets are an important field of study, as they may contribute to the mass and energy transfer from the lower to the upper atmosphere. We use the Interface Region Imaging Spectrograph (IRIS) and Solar Dynamic Observatory (SDO) observations to study two small-scale jets originating in the same on-disk coronal hole observed in October 2013. We combine dopplergrams, intensity maps, and line width maps derived from IRIS Si IV 1393.755 $\r{A}$ spectra along with images from the Atmospheric Imaging Assembly (AIA) on SDO to describe the dynamics of the jets. Images from AIA, with the use of the emission measure loci technique and rectangular differential emission measure (DEM) distributions, provide estimations of the plasma temperatures. We used the O IV 1399.77 $\r{A}$, 1401.16 $\r{A}$ spectral lines from IRIS to derive electron densities. For jet 1, the SDO images show a small mini-filament 2 minutes before the jet eruption, while jet 2 originates at a pre-existing coronal bright point. The analysis of asymmetric spectral profiles of the Si IV 1393.755 $\r{A}$ and 1402.770 $\r{A}$ lines reveals the existence of two spectral components with inversely dependant 1393.755 $\r{A}$/1402.770 $\r{A}$ ratios at both regions. One of the components can be related to the background plasma emission originating outside the jet, while the secondary component represents higher-energy plasma flows associated with the jets. Both jets exhibit high densities of the order of 10$^{11}$ cm$^{-3}$ at their base and 10$^{10}$ cm$^{-3}$ at the spire, respectively, as well as similar average nonthermal velocities of $\sim$ 50-60 km/s. However, the two jets show differences in their length, duration, and plane-of-sky velocity. Finally, the DEM analysis reveals that both jets exhibit multithermal distributions.