Observations of solar X-ray and EUV jets and their related phenomena

TL;DR

This paper reviews solar X-ray and EUV jets, their characteristics, origins, and their role in solar phenomena, emphasizing how their features depend on magnetic field configurations and their potential contribution to solar wind.

Contribution

It provides a comprehensive overview of the observational features and underlying mechanisms of solar jets, highlighting the influence of magnetic environments on jet properties.

Findings

Jets are associated with magnetic reconnection and vary with magnetic environment.

Large jets can produce type III radio bursts and energetic particles.

Jet features like repetition rate depend on photospheric magnetic configurations.

Abstract

Solar jets are fast-moving, elongated brightenings related to ejections seen in both images and spectra on all scales from barely visible chromospheric jets to coronal jets extending up to a few solar radii. The largest, most powerful jets are the source of type III radio bursts, energetic electrons and ions with greatly enhanced $^3$He and heavy element abundances. The frequent coronal jets from polar and equatorial coronal holes may contribute to the solar wind. The primary acceleration mechanism for all jets is believed to be release of magnetic stress via reconnection; however the energy buildup depends on the jets' source environment. In this review, we discuss how certain features of X-ray and EUV jets, such as their repetition rate and association with radio emission, depends on their underlying photospheric field configurations (active regions, polar and equatorial coronal holes, and quiet Sun).