Abstract
Abstract Coronal cavities have previously been observed to be associated with long-lived quiescent filaments and are thought to correspond to the associated magnetic flux rope. Although the standard flare model predicts a coronal cavity corresponding to the erupting flux rope, these have only been observed using broadband imaging data, restricting an analysis to the plane-of-sky. We present a unique set of spectroscopic observations of an active region filament seen erupting at the solar limb in the extreme ultraviolet. The cavity erupted and expanded rapidly, with the change in rise phase contemporaneous with an increase in nonthermal electron energy flux of the associated flare. Hot and cool filamentary material was observed to rise with the erupting flux rope, disappearing suddenly as the cavity appeared. Although strongly blueshifted plasma continued to be observed flowing from the apex of the erupting flux rope, this outflow soon ceased. These results indicate that the sudden injection of energy from the flare beneath forced the rapid eruption and expansion of the flux rope, driving strong plasma flows, which resulted in the eruption of an under-dense filamentary flux rope.
Highlights
Solar eruptions are the most energetic and spectacular events that occur in the solar system
The combination of spectroscopic Extreme ultraviolet Imaging Spectrometer (EIS) and broadband Atmospheric Imaging Assembly (AIA) observations presented here describe the very fast eruption of a coronal cavity with a mixed temperature outer sheath and containing a combination of hot and cool plasma that exhibited very strong blue-shifts. This is a unique set of observations and as such requires some examination to determine the physical processes at work
The temporal evolution of the coronal cavity obtained using the images from Solar Dynamics Observatory (SDO)/AIA indicates that the cavity initially began to rise slowly
Summary
Solar eruptions are the most energetic and spectacular events that occur in the solar system. The existence of a pre-eruptive flux rope configuration can be inferred through the observations of dark cavities in white light, extreme ultraviolet (EUV) and X-ray observations when located at or near the solar limb (cf Gibson et al 2006; Habbal et al 2010; Kucera et al 2012; Reeves et al 2012; Karna et al 2015). Limb observations of eruptive events, using emission measure analysis techniques, have revealed magnetic flux ropes with a hot, bright sheath surrounding a cool, dark cavity which contains a hot, bright core (cf Hannah & Kontar 2013; Kumar & Cho 2014; Lee et al 2017).
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
