The Coronal-dimming Footprint Of A Streamer-puff Coronal Mass Ejection: Confirmation Of The Magnetic-arch-blowout Scenario

Details The Coronal-dimming Footprint Of A Streamer-puff Coronal Mass Ejection: Confirmation Of The Magnetic-arch-blowout Scenario The Coronal-dimming Footprint Of A Streamer-puff Coronal Mass Ejection: Confirmation Of The Magnetic-arch-blowout Scenario

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2907m&link_type=abstract

American Astronomical Society Meeting 210, #29.07; Bulletin of the American Astronomical Society, Vol. 39, p.138

Physics

Scientific paper

A streamer puff is a recently identified variety of coronal mass ejection (CME) of narrow to moderate width. It (1) travels out along a streamer, transiently inflating the streamer but leaving it largely intact, and (2) occurs in step with a compact ejective flare in an outer flank of the base of the streamer. These aspects suggest the following magnetic-arch-blowout scenario for the production of these CMEs: the magnetic explosion that produces the flare also produces a plasmoid that explodes up the leg of an outer loop of the arcade base of the streamer, blows out the top of this loop, and becomes the core of the CME. In this paper, we present a steamer-puff CME that produced a coronal dimming footprint. The coronal dimming, its magnetic setting, and the timing and magnetic setting of a strong compact ejective flare within the dimming footprint nicely confirm the magnetic-arch-blowout scenario. From these observations, together with several published cases of a trans-equatorial CME produced in tandem with an ejective flare or filament eruption that was far offset from directly under the CME, we propose the following. Streamer-puff CMEs are a subclass (one variety) of a broader class of “over-and-out” CMEs that are often much larger than steamer puffs but are similar to them in that they are produced by the blowout of a large quasi-potential magnetic arch by a magnetic explosion that erupts from one foot of the large arch, where it is marked by a filament eruption and/or an ejective flare.
This work was funded by the Heliophysics Division of NASA's Science Mission Directorate.

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