Large-scale phenomena on the Sun associated with the eruption of filaments outside active regions: the event of September 12, 1999

Details Large-scale phenomena on the Sun associated with the eruption of filaments outside active regions: the event of September 12, 1999 Large-scale phenomena on the Sun associated with the eruption of filaments outside active regions: the event of September 12, 1999

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009arep...53..355c&link_type=abstract

Astronomy Reports, Volume 53, Issue 4, pp.355-368

Astronomy and Astrophysics

Astronomy

1

96.60.Qf, 96.60.Ph

Scientific paper

The event of September 12, 1999 is used to analyze large-scale disturbances associated with coronal mass ejections during the eruption of filaments outside active regions. The analysis is based on H α filtergrams, EUV and soft X-ray images, and coronograph data. The filament eruption occurred in relatively weak magnetic fields, but was accompanied by larger-scale phenomena than flare events. During several hours after the eruption, a large-scale arcade developed, whose bases formed diverging flare-like ribbons. The volume of the event was bounded by an “EIT wave”, which was quasi-stationary at the solar surface and expanded above the limb. The event did not have an impulsive component; therefore the “EIT wave” above the limb was a magnetic structure, identified as the front of a coronal mass ejection by virtue of its shape, structural features, and kinematics. Three types of dimmings were observed within the areal of the event, cause by (a) the evacuation of plasma, (b) heating of plasma with its subsequent evacuation, and (c) the absorption of radiation in a system of filaments activated by the eruption. The fact that a dimming appeared due to plasma heating was revealed by its presence in soft X-rays, whereas the four EIT channels did not demonstrate this. This brings into question the correctness of certain conclusions drawn earlier based purely on EIT data. A transformation of magnetic fields brought about by the eruption also occurred in a stationary coronal hole adjacent to the areal of the event. The expansion of the coronal mass ejection was self-similar and characterized by a rapidly decreasing acceleration, which is not taken into account in the widely used polynomial approximation.

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