Multiwavelength Study of 24 Equatorial Coronal-Hole Jets
Abstract
Coronal jets are transient/collimated plasma ejections that repeatedly occur in coronal holes and contribute mass/energy to solar wind and corona. By combining numerical simulations and high-resolution observations, we have made substantial progress recently on determining the energy build-up and release processes in these jets. Here we describe a study of 24 equatorial coronal-hole jets using SDO/AIA and HMI observations on January 2014. Out of 24 jets, 16 (67%) are associated with mini-filament eruptions and 8 (34%) do not show mini-filament eruptions but do exhibit mini-flare arcades and other CME-like signatures, indicating that every jet in our sample involved a filament-channel eruption. From the complete set of events, 5 jets (21%) are apparently associated with tiny flux-cancellation events at the polarity inversion line, and 3 events are associated with sympathetic eruptions of filaments from neighboring jet sources. Potential field extrapolations of the source regions reveal that almost all jets occurred in the fan-spine topology, and are in agreement with the breakout model of solar eruptions (Wyper et al. 2017). We present selected examples of each type, and discuss the implications for the jet energy buildup and initiation mechanisms.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2018
- Bibcode:
- 2018AGUFMSH13A..03K