Observations of solar X‐ray and EUV jets and their related phenomena. Issue 10 (29th November 2016)

• Record Type: Journal Article
• Authors: Innes, D. E.; Bučík, R.; Guo, L.‐J.; Nitta, N.
• Other Names: Louis R. sponsoringEditor.; Mann G. sponsoringEditor.; Denker C. sponsoringEditor.
• Is Part Of: Astronomische Nachrichten. Volume 337:Issue 10(2016)
• Page Start: 1024
• Page End: 1032
• Publication Date: 2016-11-29
• Subjects: Sun: activity -- Sun: magnetic field -- Sun: particle emission -- Sun: X‐rays; Astronomy -- Periodicals; 520.5
• DOI: 10.1002/asna.201612428
• Languages: English
• ISSNs: 0004-6337

Abstract

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). (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)