Filament Eruptions During the Period of Sept. 1991 through Sept. 1994

Details Filament Eruptions During the Period of Sept. 1991 through Sept. 1994 Filament Eruptions During the Period of Sept. 1991 through Sept. 1994

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997spd....28.0103k&link_type=abstract

American Astronomical Society, SPD meeting #28, #01.03; Bulletin of the American Astronomical Society, Vol. 29, p.879

Astronomy and Astrophysics

Astronomy

Scientific paper

From Sept. 1, 1991 to Sept 12, 1994, full disk Hα images were recorded continuously at Big Bear Solar Observatory (BBSO) by super-VHS video recorder. We digitized one image every half hour for that entire period when the BBSO data are available. About 10,000 halpha images are archived online, so anybody in the community can have an access to such an archive, which are useful in studying the evolution of solar active regions, flares and filament eruptions. In particular, we are interested in the statistical properties of solar filaments based on this set of data. In this paper, we present a complete list of filament disappearance. In the first table, we list the disk location, size and the time of disappearance of all significant filaments with a minimum length of 70.1 arcsec. In the second table, we list above properties of all the detectable filaments for the period of Jan. 1994 to Sept. 1994. The filaments disappear in four different ways: (1) erupt during continuous observations, so its disappearance time is accurate to within half hour. (2) disappear during the BBSO night gap (12 to 14 hours); (3) disappear during date gap (most likely due to bad weather) and (4) rotate beyond the West limb.

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