Coronal jets, magnetic topologies, and the production of interplanetary electron streams

Abstract

We investigate the acceleration source of the impulsive solar energetic particle (SEP) events on 2007 January 24. Combining the in situ electron measurements and remote-sensing solar observations, as well as the calculated magnetic fields obtained from a potential-field source-surface model, we demonstrate that the jets associated with the hard X-ray flares and type-III radio bursts, rather than the slow and partial coronal mass ejections, are closely related to the production of interplanetary electron streams. The jets, originated from the well-connected active region (AR 10939) whose magnetic polarity structure favors the eruption, are observed to be forming in a coronal site, extending to a few solar radii, and having a good temporal correlation with the electron solar release. The open-field lines near the jet site are rooted in a negative polarity, along which energetic particles escape from the flaring AR to the near-Earth space, consistent with the in situ electron pitch angle distribution. The analysis enables us to propose a coronal magnetic topology relating the impulsive SEP events to their solar source.

References in corpus (1)

• Major electron events and coronal magnetic configurations of the related solar active regions

Cited by in corpus (6)

• Observation and Modeling of Solar Jets
• Electron and proton acceleration during the first ground level enhancement of solar cycle 24
• Multi-Spacecraft Observations of Recurrent 3He-Rich Solar Energetic Particles
• Waiting time distribution of solar energetic particle events modeled with a non-stationary Poisson process
• Three-stage Acceleration of Solar Energetic Particles Detected by Parker Solar Probe
• Coronal magnetic topology and the production of solar impulsive energetic electrons