Observations of the Merging of Two Quiescent Filaments

Details Observations of the Merging of Two Quiescent Filaments Observations of the Merging of Two Quiescent Filaments

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.5302m&link_type=abstract

American Astronomical Society Meeting 210, #53.02; Bulletin of the American Astronomical Society, Vol. 39, p.164

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Scientific paper

The two filaments were observed close to disk center in the same field of view of approximately 9x9 arc. min. The observations were made using a tunable lithium niobate, narrow band etalon on the 25 cm Martin Solar Telescope at Helio Research in southern California. One filament was close to the equator and was oriented nearly east-west and the other, to the west, was oriented north-south with the north end approximately 120 Mm from the west end of the equatorial filament. Continued observations were made of these filaments for 2 to 5.5 hours per day between October 10 and 15, 2004. The observations were made at multiple wavelengths within + and - 1 Å around Hα.
We compared Hα centerline images with data taken by SOHO/EIT at 304A and observed significant differences in the evolution of the filaments at these wavelengths. For example, in EIT 304 Å images the two filaments seem to join on October 12, i.e. about two days earlier than in Hα. Moreover, the observed merging took longer (over three days) in Hα than in EIT 304 Å images, where it took place on a single day. The dynamics of the merger event is demonstrated with Hα and EIT 304 Å movies.
The Doppler velocities calculated from the line wings images before, during and after the merging event were in the normal range for quiescent filaments. In our investigation of subsequent SOHO/EIT images at 304 Å we found no sign of an eruption due to the merging of the filaments.
The contribution of KM was supported under NASA grant NAG5-10852 and SFM acknowledges NSF grant ATM-0519249.

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