Erupting Chromospheric Filaments

Details Erupting Chromospheric Filaments Erupting Chromospheric Filaments

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1010b&link_type=abstract

American Astronomical Society, SPD meeting #40, #10.10; Bulletin of the American Astronomical Society, Vol. 41, p.824

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Erupting filaments are commonly associated with coronal mass ejections. They represent the chromospheric structures most closely tied to the underlying photospheric magnetic fields. We present an analysis of the eruption of an unusually large filament on the SE quadrant of the solar disc on 2003 June 11. The data are drawn from USAF/NSO Improved Solar Observing Optical Network, Solar and Heliospheric Observatory, and ground-based telescopes at NSO. The filament rises with an initial slow speed of 6-7 km/s over a period of 2 hours and later erupts by rapidly accelerating to 170 km/s second in the following 30 minutes. The filament eruption is accompanied by a flare in a neighboring active region. We trace morphological and topological changes in the filament and overlying arcade before and during its eruption, and interpret these changes in terms of physical structure of the filament and whole filament system. The destabilization of the filament and its overlying coronal arcade are related to interactions with a new emerging active region, and adjacent active region.

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