3He-Rich Solar Energetic Particles in Helical Jets on the Sun

Particle acceleration in stellar flares is ubiquitous in the Universe, however, our Sun is the only astrophysical object where energetic particles and their source flares can both be observed. The acceleration mechanism in solar flares, tremendously enhancing (up to a factor of ten thousand) rare el...

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Bibliographic Details
Published in:arXiv.org 2017-11
Main Authors: Bucik, Radoslav, Innes, Davina E, Mason, Glenn M, Wiedenbeck, Mark E, Gomez-Herrero, Raul, Nitta, Nariaki V
Format: Article
Language:English
Subjects:
Coronal hole boundaries
Energetic particles
Heavy nuclei
Image resolution
Iron
Jets
Observatories
Particle acceleration
Solar activity
Solar corona
Solar flares
Solar radio bursts
Stellar flares
Sun
Universe
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Summary:Particle acceleration in stellar flares is ubiquitous in the Universe, however, our Sun is the only astrophysical object where energetic particles and their source flares can both be observed. The acceleration mechanism in solar flares, tremendously enhancing (up to a factor of ten thousand) rare elements like 3He and ultra-heavy nuclei, has been puzzling for almost 50 years. Here we present some of the most intense 3He- and Fe-rich solar energetic particle events ever reported. The events were accompanied by non-relativistic electron events and type III radio bursts. The corresponding high-resolution, extreme-ultraviolet imaging observations have revealed for the first time a helical structure in the source flare with a jet-like shape. The helical jets originated in relatively small, compact active regions, located at the coronal hole boundary. A mini-filament at the base of the jet appears to trigger these events. The events were observed with the two Solar Terrestrial Relations Observatories STEREO on the backside of the Sun, during the period of increased solar activity in 2014. The helical jets may be a distinct feature of these intense events that is related to the production of high 3He and Fe enrichments.
ISSN:2331-8422
DOI:10.48550/arxiv.1711.09394