Journal
SPACE SCIENCE REVIEWS
Volume 201, Issue 1-4, Pages 1-53Publisher
SPRINGER
DOI: 10.1007/s11214-016-0260-5
Keywords
Plasmas; Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation; Sun: X-rays
Categories
Funding
- FP7 Marie Curie Grant [FP7-PEOPLE-2010-RG/268288]
- European Union (European Social Fund-ESF)
- Greek national funds through the Operational Program Education and Lifelong Learning of the National Strategic Reference Framework (NSRF)-Research Funding Program: Thales
- Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program
- Hinode Project Office at NASA/MSFC
- National Science Foundation [AGS-1159353]
- NASA
- Computational and Information Systems Laboratory
- HAO
- AFOSR [FA9550-15-1-0030]
- Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract
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Coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of nominal solar flares and coronal mass ejections (CMEs), jets share many common properties with these phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems.
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